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NGC 4325

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NGC4325
SDSSimage of NGC 4325.
Observation data (J2000epoch)
ConstellationVirgo
Right ascension12h23m06.7s[1]
Declination10° 37′ 16″[1]
Redshift0.025489[1]
Heliocentric radial velocity7641 km/s[1]
Distance330Mly(102Mpc)[1]
GrouporclusterNGC 4325 Group
Apparent magnitude(V)14.2[1]
Absolute magnitude(V)-22.12[2]
Characteristics
TypeE4[1]
Mass1.31×1011(Stellar mass)/9×1012(Total Mass)[2]M☉
Size~133,900ly(41.05kpc) (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 4325is anelliptical galaxylocated about 330 millionlight-yearsaway[3]in the constellationVirgo.It was discovered by astronomerHeinrich d'Arreston 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 theVirgo Clusterbut instead a background galaxy.[5]

Physical characteristics

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

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

AGN activity

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Observations by theROSATandChandra X-rayspace telescopes reveal that a result of pastAGNactivity in NGC 4325, there exist X-ray cavities in theICMof theNGC 4325 Group.[12][13]These two small X-ray cavities with a diameter of around 16,000ly(5kpc), 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 23,000ly(7kpc) 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 98,000ly(30kpc) 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 inX-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 9,800ly(3kpc) 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 theIGM,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 ametal-richelongated 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 agalactic wind.[15]

Supermassive Black Hole

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

Nearby Galaxies

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NGC 4325 is a member of theNGC 4325 Group,[17]which is part of theComa Supercluster.[18]The NGC 4325 Group contains 28 confirmed members[19]includingNGC 4320which is apeculiar galaxy.[17]The NGC 4325 Group has a velocity dispersion of around 298 km and a mass of 3.2×1013solar masses.The presence of ametal-richelongated 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 1,600,000ly(0.5Mpc) from the center of the group suggest that the NGC 4325 Group is dynamically young and will evolve over time thoughgalaxy mergers.[15]

See also

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References

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  1. ^abcdefghij"NASA/IPAC Extragalactic Database".Results for NGC 4325.Retrieved2022-03-03.
  2. ^abHarris, 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.ISSN0004-637X.
  3. ^"Your NED Search Results".ned.ipac.caltech.edu.Retrieved2024-06-17.
  4. ^"NGC/IC Project Restoration Efforts".ngcicproject.observers.org.Retrieved2024-06-17.
  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.ISSN0004-637X.
  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.ISSN0004-6256.
  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.ISSN0004-637X.
  9. ^abcMcDonald, 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.ISSN0004-637X.
  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.ISSN0004-6256.
  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)."ChandraEarly-type Galaxy Atlas ".The Astrophysical Journal Supplement Series.241(2): 36.arXiv:1812.02718.Bibcode:2019ApJS..241...36K.doi:10.3847/1538-4365/ab0ca4.ISSN1538-4365.
  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.ISSN0004-6361.
  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.ISSN0004-637X.
  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.ISSN0035-8711.
  15. ^abLaganá, 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.ISSN0004-6361.
  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.ISSN0004-637X.
  17. ^abHelsdon, 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.ISSN0035-8711.
  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.ISSN0004-6361.
  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.ISSN0004-637X.
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