NGC 5643
{{Short description|Galaxy in the constellation Lupus}}
{{Infobox galaxy
| name = NGC 5643
| image =NGC 5643.png
| caption = NGC 5643 imaged by the Hubble Space Telescope
| epoch = J2000
| type = SAB(rs)c {{cite web
| title=NASA/IPAC Extragalactic Database
| work=Results for NGC 5643
| url=http://ned.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=NGC+5643
| access-date=2016-01-18 }}
| appmag_v = 10.7
| size_v = 4.6{{prime}} × 4.0{{prime}}
| constellation name = Lupus
| notes =
| names = ESO 272- G 016, MCG -07-30-003, PGC 51969
}}
NGC 5643 is an intermediate spiral galaxy in the constellation Lupus. Based on the tip of the red-giant branch distance indicator, it is located at a distance of about 40 million light-years (12.5 megaparsecs). NGC 5643 has an active galactic nucleus and is a type II Seyfert galaxy.
Observation history
The galaxy was first discovered by James Dunlop on May 10, 1826, with his 9-inch reflector telescope, who described it as exceedingly faint. The galaxy was also spotted by John Herschel and added to the General Catalogue of Nebulae and Clusters as number 3572. The galaxy is located only 15 degrees from the galactic plane.{{cite book|last1=O'Meara|first1=Stephen James|title=Southern gems|date=2013|publisher=Cambridge University Press|location=Cambridge|isbn=978-1107015012|pages=272|ref=Meara}}
Structure
NGC 5643 is a grand design spiral galaxy, with two well-defined, symmetric arms. In the circumnuclear region are other dust spirals, but the two main dust arms are wider.{{cite journal|last1=Martini|first1=Paul|last2=Regan|first2=Michael W.|last3=Mulchaey|first3=John S.|last4=Pogge|first4=Richard W.|title=Circumnuclear Dust in Nearby Active and Inactive Galaxies. I. Data|journal=The Astrophysical Journal Supplement Series|date=June 2003|volume=146|issue=2|pages=353–406|doi=10.1086/367817|arxiv=astro-ph/0212396|bibcode=2003ApJS..146..353M|s2cid=15161097}} The galaxy is seen nearly face on, at an inclination of ~ 27°.
= Active galactic nucleus =
File:Center of galaxy NGC 5643.tif and VLT.{{cite web|title=Hidden from view|url=https://www.eso.org/public/images/potw1822a/|website=www.eso.org|access-date=28 May 2018}}]]
The galaxy has a low-luminosity active galactic nucleus of Seyfert 2 type and is also a luminous infrared galaxy. The galaxy has a double sided diffuse radiojet. The galaxy exhibits an extended emission line region elongated in a direction close to the radio position angle of 87°±3°. Chris Simpson et al. analysed images takes from the WFPC2 camera of the Hubble Space Telescope in [O III] λ5007 and Hα and found emission extending eastward for at least 1.8 kpc and in the [O III]/Hα map a well-defined V-shaped structure that they identified as the projection of a tridimensional ionisation cone, which shares the same axis with the radio emission. A dust lane perpendicular to this axis obstructs the nucleus from direct view.{{cite journal|last1=Simpson|first1=Chris|last2=Wilson|first2=A. S.|last3=Bower|first3=Gary|last4=Heckman|first4=T. M.|last5=Krolik|first5=J. H.|last6=Miley|first6=G. K.|title=A One-sided Ionization Cone in the Seyfert 2 Galaxy NGC 5643|journal=The Astrophysical Journal|date=January 1997|volume=474|issue=1|pages=121–128|doi=10.1086/303466|bibcode=1997ApJ...474..121S|doi-access=free}} A disk of material was found when the data cubes of VLT were analysed. It is aligned with the nucleus and circles it and possibly provides gas to the active galactic nucleus.{{cite journal|last1=Menezes|first1=R. B.|last2=da Silva|first2=P.|last3=Ricci|first3=T. V.|last4=Steiner|first4=J. E.|last5=May|first5=D.|last6=Borges|first6=B. W.|title=A treatment procedure for VLT/SINFONI data cubes: application to NGC 5643|journal=Monthly Notices of the Royal Astronomical Society|date=16 April 2015|volume=450|issue=1|pages=369–396|doi=10.1093/mnras/stv629|doi-access=free |arxiv=1504.02933|bibcode=2015MNRAS.450..369M}} The mass of the supermassive black hole has been estimated based on the galaxy stellar velocity dispersion to be 106.4 M⊙.{{cite journal|last1=Goulding|first1=A. D.|last2=Alexander|first2=D. M.|last3=Lehmer|first3=B. D.|last4=Mullaney|first4=J. R.|title=Towards a complete census of active galactic nuclei in nearby galaxies: the incidence of growing black holes|journal=Monthly Notices of the Royal Astronomical Society|date=21 July 2010|volume=406|issue=1|pages=597–611|doi=10.1111/j.1365-2966.2010.16700.x|doi-access=free |arxiv=1003.3015|bibcode=2010MNRAS.406..597G|s2cid=53579415}} It has been proposed that the gas outflow has led to star formation on two locations on the bar of the galaxy which lie at the location where the gas from the nucleus encounters the dense material of the bar.{{cite journal|last1=Cresci|first1=G.|last2=Marconi|first2=A.|last3=Zibetti|first3=S.|last4=Risaliti|first4=G.|last5=Carniani|first5=S.|last6=Mannucci|first6=F.|last7=Gallazzi|first7=A.|last8=Maiolino|first8=R.|last9=Balmaverde|first9=B.|last10=Brusa|first10=M.|last11=Capetti|first11=A.|last12=Cicone|first12=C.|last13=Feruglio|first13=C.|last14=Bland-Hawthorn|first14=J.|last15=Nagao|first15=T.|last16=Oliva|first16=E.|last17=Salvato|first17=M.|last18=Sani|first18=E.|last19=Tozzi|first19=P.|last20=Urrutia|first20=T.|last21=Venturi|first21=G.|title=The MAGNUM survey: positive feedback in the nuclear region of NGC 5643 suggested by MUSE|journal=Astronomy & Astrophysics|date=8 October 2015|volume=582|pages=A63|doi=10.1051/0004-6361/201526581|arxiv=1508.04464|bibcode=2015A&A...582A..63C|s2cid=55222207}}
Via observations of the galaxy from the XMM Newton telescope in 2009, the galaxy is found to have a Compton–thick active galactic nucleus. Also the galaxy emits soft X-rays, mainly from photoionized matter.{{cite journal|last1=Matt|first1=G.|last2=Bianchi|first2=S.|last3=Marinucci|first3=A.|last4=Guainazzi|first4=M.|last5=Iwawasa|first5=K.|last6=Jimenez Bailon|first6=E.|title=X-ray observations of the Compton-thick Seyfert 2 galaxy, NGC 5643|journal=Astronomy & Astrophysics|date=2 August 2013|volume=556|pages=A91|doi=10.1051/0004-6361/201321293|arxiv=1307.1591|bibcode=2013A&A...556A..91M|s2cid=53347282}} The presence of the compton-thick column which obstructs the nucleus was confirmed from observations by NuSTAR.{{cite journal|last1=Annuar|first1=A.|last2=Gandhi|first2=P.|last3=Alexander|first3=D. M.|last4=Lansbury|first4=G. B.|last5=Arévalo|first5=P.|last6=Ballantyne|first6=D. R.|last7=Baloković|first7=M.|last8=Bauer|first8=F. E.|last9=Boggs|first9=S. E.|last10=Brandt|first10=W. N.|last11=Brightman|first11=M.|last12=Christensen|first12=F. E.|last13=Craig|first13=W. W.|last14=Moro|first14=A. Del|last15=Hailey|first15=C. J.|last16=Harrison|first16=F. A.|last17=Hickox|first17=R. C.|last18=Matt|first18=G.|last19=Puccetti|first19=S.|last20=Ricci|first20=C.|last21=Rigby|first21=J. R.|last22=Stern|first22=D.|last23=Walton|first23=D. J.|last24=Zappacosta|first24=L.|last25=Zhang|first25=W.|title=NuSTAR Observations of the Compton-thick Active Galactic Nucleus and Ultraluminous X-ray Source Candidate in NGC 5643|journal=The Astrophysical Journal|date=4 December 2015|volume=815|issue=1|pages=36|doi=10.1088/0004-637X/815/1/36|arxiv=1509.03322|bibcode=2015ApJ...815...36A|s2cid=11400958}}
= Ultraluminous X-ray source =
In 2004, Guainazzi et al. detected in the images from XMM-Newton an ultraluminous X-ray source, named NGC 5643 ULX1, located within 0.8 arcminutes from the nucleus. The source outshone the nucleus in X-rays and if it is located within NGC 5643 its luminosity is over 1040 erg/s. Its luminosity is variable.{{cite journal|last1=Guainazzi|first1=M.|last2=Rodriguez-Pascual|first2=P.|last3=Fabian|first3=A. C.|last4=Iwasawa|first4=K.|last5=Matt|first5=G.|title=Unveiling the nature of the highly obscured active galactic nucleus in NGC 5643 with|journal=Monthly Notices of the Royal Astronomical Society|date=November 2004|volume=355|issue=1|pages=297–306|doi=10.1111/j.1365-2966.2004.08317.x|doi-access=free |arxiv=astro-ph/0408300|bibcode=2004MNRAS.355..297G|s2cid=119067322 }} The X-rays could be produced either by an advection dominated disc or a Comptonising corona and the X-ray source is considered to be a black hole of stellar origin of approximately 30 solar masses.{{cite journal|last1=Pintore|first1=Fabio|last2=Zampieri|first2=Luca|last3=Sutton|first3=Andrew D.|last4=Roberts|first4=Timothy P.|last5=Middleton|first5=Matthew J.|last6=Gladstone|first6=Jeanette C.|title=The ultraluminous X-ray source NGC 5643 ULX1: a large stellar mass black hole accreting at super-Eddington rates?|journal=Monthly Notices of the Royal Astronomical Society|date=11 June 2016|volume=459|issue=1|pages=455–466|doi=10.1093/mnras/stw669|doi-access=free |arxiv=1603.05542|bibcode=2016MNRAS.459..455P}}
Supernovae
Two supernovae have been recorded within the galaxy:
- SN 2013aa (type{{nbsp}}Ia, mag. 11.9) was discovered by Stuart Parker from New Zealand on 13 February 2013, as part of the Backyard Observatory Supernova Search.{{cite journal | bibcode=2013CBET.3416....1P| title=Supernova 2013aa in NGC 5643 = PSN J14323388-4413278| last1=Parker| first1=S.| last2=Amorim| first2=A.| last3=Parrent| first3=J. T.| last4=Sand| first4=D.| last5=Valenti| first5=S.| last6=Graham| first6=M. L.| last7=Howell| first7=D. A.| journal=Central Bureau Electronic Telegrams| date=2013| volume=3416| page=1}}{{cite web | website=Transient Name Server | title=SN{{nbsp}}2013aa | url=https://www.wis-tns.org/object/2013aa | publisher = IAU | access-date=6 December 2024}} It was classified as a type Ia a few days before maximum brightness.{{cite journal|last1=Sternberg|first1=A.|last2=Gal-Yam|first2=A.|last3=Simon|first3=J. D.|last4=Patat|first4=F.|last5=Hillebrandt|first5=W.|last6=Phillips|first6=M. M.|last7=Foley|first7=R. J.|last8=Thompson|first8=I.|last9=Morrell|first9=N.|last10=Chomiuk|first10=L.|last11=Soderberg|first11=A. M.|last12=Yong|first12=D.|last13=Kraus|first13=A. L.|last14=Herczeg|first14=G. J.|last15=Hsiao|first15=E. Y.|last16=Raskutti|first16=S.|last17=Cohen|first17=J. G.|last18=Mazzali|first18=P. A.|last19=Nomoto|first19=K.|title=Multi-epoch high-spectral-resolution observations of neutral sodium in 14 Type Ia supernovae|journal=Monthly Notices of the Royal Astronomical Society|date=25 July 2014|volume=443|issue=2|pages=1849–1860|doi=10.1093/mnras/stu1202|doi-access=free |arxiv=1311.3645|bibcode=2014MNRAS.443.1849S}} It got as bright as magnitude 11.3, making it the brightest supernova of the year 2013.{{cite web
| url = https://www.rochesterastronomy.org/sn2013/index.html
| title = Bright Supernovae - 2013
| last = Bishop
| first = David
| website = Rochester Astronomy
| access-date = 8 December 2024
}}
- SN 2017cbv (type{{nbsp}}Ia, mag. 16.0451) was discovered by the Distance Less Than 40 Mpc Survey (DLT40) on 10 March 2017.{{cite journal | bibcode=2017ATel10158....1T| title=The discovery of DLT17u/AT 2017cbv| last1=Tartaglia| first1=L.| last2=Sand| first2=D.| last3=Wyatt| first3=S.| last4=Valenti| first4=S.| last5=Bostroem| first5=K. A.| last6=Reichart| first6=D. E.| last7=Haislip| first7=J. B.| last8=Kouprianov| first8=V.| journal=The Astronomer's Telegram| date=2017| volume=10158| page=1}}{{cite web | website=Transient Name Server | title=SN{{nbsp}}2017cbv | url=https://www.wis-tns.org/object/2017cbv | publisher = IAU | access-date=6 December 2024}} It increased in magnitude from 15.8 to 14.8 within the next day.{{cite journal | bibcode=2017ATel10167....1C| title=Swope Photometric Observations of SN 2017cbv = DLT17u| last1=Coulter| first1=D. A.| last2=Kilpatrick| first2=C. D.| last3=Foley| first3=R. J.| last4=Anais| first4=J.| last5=Phillips| first5=M. M.| last6=Drout| first6=M. R.| last7=Madore| first7=B. F.| last8=Piro| first8=A. L.| last9=Shappee| first9=B. J.| last10=Hsiao| first10=E. Y.| journal=The Astronomer's Telegram| date=2017| volume=10167| page=1}} It got as bright as magnitude 11.5, making it the brightest supernova of the year 2017.{{cite web
| url = https://www.rochesterastronomy.org/sn2017/index.html
| title = Bright Supernovae - 2017
| last = Bishop
| first = David
| website = Rochester Astronomy
| access-date = 9 December 2024
}}
Nearby galaxies
NGC 5643 has a satellite dwarf galaxy, ESO 273-014.{{cite journal|last1=Karachentsev|first1=Igor D.|last2=Kaisina|first2=Elena I.|last3=Makarov|first3=Dmitry I.|title=Suites of Dwarfs Around Nearby Giant Galaxies|journal=The Astronomical Journal|date=3 December 2013|volume=147|issue=1|pages=13|doi=10.1088/0004-6256/147/1/13|arxiv=1310.6838|bibcode=2014AJ....147...13K|s2cid=119245124}} NGC 5643 is the largest member of a small galaxy group that also includes NGC 5530.{{cite journal|last1=Makarov|first1=Dmitry|last2=Karachentsev|first2=Igor|title=Galaxy groups and clouds in the local (z~ 0.01) Universe|journal=Monthly Notices of the Royal Astronomical Society|date=21 April 2011|volume=412|issue=4|pages=2498–2520|doi=10.1111/j.1365-2966.2010.18071.x|doi-access=free |arxiv=1011.6277|bibcode=2011MNRAS.412.2498M|s2cid=119194025}}
References
{{reflist}}
External links
{{commons category}}
{{wikiSky}}
{{Ngc60}}
{{Lupus (constellation)}}
Category:Barred spiral galaxies
Category:Lupus (constellation)
Category:Galaxies discovered in 1826