NGC 4325

Last updated
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 million 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 contains 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

<span class="mw-page-title-main">Messier 60</span> Elliptical galaxy in the constellation Virgo

Messier 60 or M60, also known as NGC 4649, is an elliptical galaxy approximately 57 million light-years away in the equatorial constellation of Virgo. Together with NGC 4647, it forms a pair known as Arp 116. Messier 60 and nearby elliptical galaxy Messier 59 were discovered by Johann Gottfried Koehler in April 1779, observing a comet in the same part of the sky. Charles Messier added both to his catalogue about three days after this.

<span class="mw-page-title-main">MS 0735.6+7421</span> Galaxy cluster in the constellation Camelopardalis

MS 0735.6+7421 is a galaxy cluster located in the constellation Camelopardalis, approximately 2.6 billion light-years away. It is notable as the location of one of the largest central galactic black holes in the known universe, which has also apparently produced one of the most powerful active galactic nucleus eruptions discovered.

<span class="mw-page-title-main">NGC 1042</span> Spiral galaxy in the constellation Cetus

NGC 1042 is a spiral galaxy located in the constellation Cetus. It was discovered on 10 November 1885 by American astronomer Lewis Swift. The galaxy has an apparent magnitude of 14.0.

<span class="mw-page-title-main">NGC 4309</span> Galaxy in the constellation Virgo

NGC 4309 is a lenticular galaxy located about 55 million light-years away in the constellation Virgo. The galaxy was discovered by astronomer Christian Peters in 1881 and is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 4323</span> Galaxy in the constellation Coma Berenices

NGC 4323 is a lenticular or dwarf elliptical galaxy located about 52.5 million light-years away in the constellation Coma Berenices. The galaxy was discovered in 1882 by astronomer Wilhelm Tempel and is a member of the Virgo Cluster.

<span class="mw-page-title-main">RX J1532.9+3021</span> Galaxy cluster in the constellation Corona Borealis

RX J1532.9+3021 is a galaxy cluster located in the constellation of Corona Borealis. It has a velocity of 103,539 ± 8 kilometers per second, equivalent to a Hubble distance of 1,527.1 ± 106.9 megaparsecs or 3.9 billion light years. It is classfied one of the massive and strongest X-ray bright cool clusters in the universe at redshift z = 0.362. The luminosity of the cluster is estimated to be 6 x 1045 ergs-1. According to a study published in 2013, a mini radio halo is seen surrounding the cluster.

<span class="mw-page-title-main">NGC 4388</span> Galaxy in the constellation Virgo

NGC 4388 is an active spiral galaxy in the equatorial constellation of Virgo. It was discovered April 17, 1784 by Wilhelm Herschel. This galaxy is located at a distance of 57 million light years and is receding with a radial velocity of 2,524km/s. It is one of the brightest galaxies of the Virgo Cluster due to its luminous nucleus. NGC 4388 is located 1.3° to the west of the cluster center, which translates to a projected distance of ≈400 kpc.

<span class="mw-page-title-main">NGC 4607</span> Galaxy in the constellation Virgo

NGC 4607 is an edge-on spiral galaxy located about 56 million light-years away in the constellation Virgo. NGC 4607 was discovered by astronomer R. J. Mitchell on April 24, 1854. The galaxy is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 4660</span> Galaxy in the constellation Virgo

NGC 4660 is an elliptical galaxy located about 63 million light-years away in the constellation Virgo. The galaxy was discovered by astronomer William Herschel on March 15, 1784 and is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 708</span> Galaxy in the constellation Andromeda

NGC 708 is an elliptical galaxy located 240 million light-years away in the constellation Andromeda and was discovered by astronomer William Herschel on September 21, 1786. It is classified as a cD galaxy and is the brightest member of Abell 262. NGC 708 is a weak FR I radio galaxy and is also classified as a type 2 Seyfert galaxy.

<span class="mw-page-title-main">NGC 4636</span> Galaxy in the constellation Virgo

NGC 4636 is an elliptical galaxy located in the constellation Virgo. It is a member of the NGC 4753 Group of galaxies, which is a member of the Virgo II Groups, a series of galaxies and galaxy clusters strung out from the southern edge of the Virgo Supercluster. It is located at a distance of about 55 million light years from Earth, which, given its apparent dimensions, means that NGC 4636 is about 105,000 light years across.

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

NGC 5846 is an elliptical galaxy located in the constellation Virgo. It is located at a distance of circa 90 million light years from Earth, which, given its apparent dimensions, means that NGC 5846 is about 110,000 light years across. It was discovered by William Herschel on February 24, 1786. It lies near 110 Virginis and is part of the Herschel 400 Catalogue. It is a member of the NGC 5846 Group of galaxies, itself one of the Virgo III Groups strung out to the east of the Virgo Supercluster of galaxies.

<span class="mw-page-title-main">NGC 4294</span> Galaxy in the constellation Virgo

NGC 4294 is a barred spiral galaxy with flocculent spiral arms located about 55 million light-years away in the constellation Virgo. The galaxy was discovered by astronomer William Herschel on March 15, 1784 and is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 4298</span> Galaxy in the constellation Coma Berenices

NGC 4298 is a flocculent spiral galaxy located about 53 million light-years away in the constellation Coma Berenices. The galaxy was discovered by astronomer William Herschel on April 8, 1784 and is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 4302</span> Galaxy in the constellation Coma Berenices

NGC 4302 is an edge-on spiral galaxy located about 55 million light-years away in the constellation Coma Berenices. It was discovered by astronomer William Herschel on April 8, 1784 and is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 4318</span> Galaxy in the constellation Virgo

NGC 4318 is a small lenticular galaxy located about 72 million light-years away in the constellation Virgo. It was discovered by astronomer John Herschel on January 18, 1828. NGC 4318 is a member of the Virgo W′ group, a group of galaxies in the background of the Virgo Cluster that is centered on the giant elliptical galaxy NGC 4365.

<span class="mw-page-title-main">Teacup galaxy</span> Low redshift quasar in the constellation Boötes

The Teacup galaxy, also known as the Teacup AGN or SDSS J1430+1339 is a low redshift type 2 quasar, showing an extended loop of ionized gas resembling a handle of a teacup, which was discovered by volunteers of the Galaxy Zoo project and labeled as a Voorwerpje.

<span class="mw-page-title-main">NGC 4326</span> Barred spiral galaxy in the constellation of Virgo

NGC 4326 is a barred spiral galaxy with a ring located about 330 million light-years away in the constellation Virgo. It was discovered by astronomer William Herschel on April 13, 1784, who described it as "vF, S, R, bM, 1st of 3". It is a large galaxy, with a diameter of around 200,000 ly (61 kpc) making it nearly twice the size of the Milky Way. NGC 4326 is also classified as a LINER galaxy. Despite being listed in the Virgo Cluster catalog as VCC 623, it is not a member of the Virgo Cluster but instead a background galaxy.

<span class="mw-page-title-main">IC 3528</span> Galaxy in the constellation Coma Berenices

IC 3528 is spiral galaxy located 660 million light-years away in the constellation of Coma Berenices. It lies near to another spiral galaxy NGC 4540, although the two of them are quite far. The object was discovered by Royal Harwood Frost on May 7, 1904. Although listed as a member in the Virgo Cluster Catalogue as VCC 1593, it is not a member of the Virgo cluster but a background galaxy.

<span class="mw-page-title-main">4C+55.16</span> Seyfert 2 galaxy in the constellation Ursa Major

4C+55.16 is an elliptical galaxy, classified type E, located in Ursa Major. The galaxy lies about 2.84 billion light-years from Earth, which means given its apparent dimensions, 4C+55.16 is approximately 445,000 light-years across making it a type-cD galaxy. It is the brightest cluster galaxy (BCG) in a cluster of the same name.

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.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.