NGC 5701

The galaxy is categorised as a barred lenticular galaxy. The bar is faint and diffuse, and almost completely dust-free. At its ends it has elevated brightness, forming ansae.Sandage, A., Bedke, J. (1994), The Carnegie Atlas of Galaxies. Volume I, Carnegie Institution of Washington It surrounds a large, bright and slightly elliptical bulge with a bright nucleus. The bar lies inside a disk which mostly lacks features, with the exception of some knots or possible companion galaxies.{{cite journal |last1=Eskridge |first1=Paul B. |last2=Frogel |first2=Jay A. |last3=Pogge |first3=Richard W. |last4=Quillen |first4=Alice C. |last5=Berlind |first5=Andreas A. |last6=Davies |first6=Roger L. |last7=DePoy |first7=D. L. |last8=Gilbert |first8=Karoline M. |last9=Houdashelt |first9=Mark L. |last10=Kuchinski |first10=Leslie E. |last11=Ramirez |first11=Solange V. |last12=Sellgren |first12=K. |last13=Stutz |first13=Amelia |last14=Terndrup |first14=Donald M. |last15=Tiede |first15=Glenn P. |title=Near-Infrared and Optical Morphology of Spiral Galaxies |journal=The Astrophysical Journal Supplement Series |date=November 2002 |volume=143 |issue=1 |pages=73–111 |doi=10.1086/342340|arxiv=astro-ph/0206320 |bibcode=2002ApJS..143...73E }} The bar is strong and dominates the disk, while the bulge component could overlap with the disk, making the galaxy appear to lack a disk. The lack of disk however could be the result of a model that lacks the bar as different models indicate the presence of the disk.{{cite journal |last1=Alexei Gadotti |first1=Dimitri |title=Image decomposition of barred galaxies and AGN hosts |journal=Monthly Notices of the Royal Astronomical Society |date=February 2008 |volume=384 |issue=1 |pages=420–439 |doi=10.1111/j.1365-2966.2007.12723.x|doi-access=free |arxiv=0708.3870 |bibcode=2008MNRAS.384..420G }} An inner ring is detectable at the end of the bar.{{cite journal |last1=Gadotti |first1=D. A. |last2=de Souza |first2=R. E. |title=NGC 4608 and NGC 5701: Barred Galaxies without Disks? |journal=The Astrophysical Journal |date=1 February 2003 |volume=583 |issue=2 |pages=L75–L78 |doi=10.1086/368159|arxiv=astro-ph/0301072 |bibcode=2003ApJ...583L..75G }}

The stellar population in the barlens is mostly old, as 70–85% of the stellar mass is older than 10 billion years. The intermediate age stars are more common at the outer edges of the barlens. The bar doesn't show to induse star formation. At the centre the metallicity is solar and becomes subsolar towards the edges, and is higher than that of the bulge of the Milky Way.{{cite journal |last1=Laurikainen |first1=E. |last2=Salo |first2=H. |title=Barlenses and X-shaped features compared: two manifestations of boxy/peanut bulges |journal=Astronomy & Astrophysics |date=February 2017 |volume=598 |pages=A10 |doi=10.1051/0004-6361/201628936|arxiv=1609.01936 |bibcode=2017A&A...598A..10L }} Gas and stellar velocity fields are slightly offset with each other as indicated by the position angles of their major axes.{{cite journal |last1=Seidel |first1=M. K. |last2=Falcón-Barroso |first2=J. |last3=Martínez-Valpuesta |first3=I. |last4=Díaz-García |first4=S. |last5=Laurikainen |first5=E. |last6=Salo |first6=H. |last7=Knapen |first7=J. H. |title=The BaLROG project – I. Quantifying the influence of bars on the kinematics of nearby galaxies |journal=Monthly Notices of the Royal Astronomical Society |date=21 July 2015 |volume=451 |issue=1 |pages=936–973 |doi=10.1093/mnras/stv969|doi-access=free |arxiv=1504.08001 }} The isophotes indicate that the bar is also misaligned with the stellar velocity field.{{cite journal |last1=Seidel |first1=M. K. |last2=Cacho |first2=R. |last3=Ruiz-Lara |first3=T. |last4=Falcón-Barroso |first4=J. |last5=Pérez |first5=I. |last6=Sánchez-Blázquez |first6=P. |last7=Vogt |first7=F. P. A. |last8=Ness |first8=M. |last9=Freeman |first9=K. |last10=Aniyan |first10=S. |title=Dissecting galactic bulges in space and time – I. The importance of early formation scenarios versus secular evolution |journal=Monthly Notices of the Royal Astronomical Society |date=21 January 2015 |volume=446 |issue=3 |pages=2837–2860 |doi=10.1093/mnras/stu2295|doi-access=free |arxiv=1411.2969 }}

The nucleus of the galaxy has been found to be active and based on its emission lines has been identified as a transitional object between an HII region and a LINER.{{cite journal |last1=Ho |first1=Luis C. |last2=Filippenko |first2=Alexei V. |last3=Sargent |first3=Wallace L. W. |title=A Search for Dwarf Seyfert Nuclei. III. Spectroscopic Parameters and Properties of the Host Galaxies |journal=The Astrophysical Journal Supplement Series |date=October 1997 |volume=112 |issue=2 |pages=315–390 |doi=10.1086/313041|arxiv=astro-ph/9704107 |bibcode=1997ApJS..112..315H }} The most accepted theory for the energy source of active galactic nuclei is the presence of an accretion disk around a supermassive black hole. The mass of the black hole in the centre of NGC 5701 is estimated to be 10^7.9 (80 million) {{solar mass|link=yes}} based on the absolute bulge magnitude.{{cite journal |last1=Dong |first1=X. Y. |last2=De Robertis |first2=M. M. |title=Low-Luminosity Active Galaxies and Their Central Black Holes |journal=The Astronomical Journal |date=March 2006 |volume=131 |issue=3 |pages=1236–1252 |doi=10.1086/499334|arxiv=astro-ph/0510694 |bibcode=2006AJ....131.1236D }}

A faint nuclear spiral is visible in images by the Hubble Space Telescope extending to about 10 arcseconds. As the galaxy is seen nearly face-on it is difficult to detect if an inner disk is present.{{cite journal |last1=Erwin |first1=Peter |last2=Sparke |first2=Linda S. |title=An Imaging Survey of Early-Type Barred Galaxies |journal=The Astrophysical Journal Supplement Series |date=June 2003 |volume=146 |issue=2 |pages=299–352 |doi=10.1086/367885|arxiv=astro-ph/0212092 |bibcode=2003ApJS..146..299E }} The nuclear spiral is associated with young stars, whose presence however is negligible as far as the total stellar mass of the bulge is concerned.

File:NGC 5701 GALEX WikiSky.jpg as observed by GALEX, with the ring glowing blue.]]

The galaxy has an outer pseudo-ring which is more visible in blue light.{{cite journal |last1=Laurikainen |first1=Eija |last2=Salo |first2=Heikki |last3=Buta |first3=Ronald |last4=Vasylyev |first4=Sergiy |title=Bar-induced perturbation strengths of the galaxies in the Ohio State University Bright Galaxy Survey - I |journal=Monthly Notices of the Royal Astronomical Society |date=December 2004 |volume=355 |issue=4 |pages=1251–1271 |doi=10.1111/j.1365-2966.2004.08410.x|doi-access=free |arxiv=astro-ph/0409503 |bibcode=2004MNRAS.355.1251L }} The ring is created by two arms which emerge from the end of the disk, but they start to branch into smaller arms, creating a ring of multiple fragmented arms. Many HII regions emitting H-alpha are visible in it, indicating it is a location of active star formation.{{cite journal |last1=Pogge |first1=Richard W. |last2=Eskridge |first2=Paul B. |title=Star formation in the disks of H I-rich S0 galaxies |journal=The Astronomical Journal |date=October 1993 |volume=106 |pages=1405 |doi=10.1086/116735|bibcode=1993AJ....106.1405P }} The ring is detached from the disk and gives the galaxy an appearance similar to Hoag's Object. It is possible that the bar prevents the gas infalling to the central region of the galaxy.{{cite journal |last1=Cortese |first1=L. |last2=Hughes |first2=T. M. |title=Evolutionary paths to and from the red sequence: star formation and H i properties of transition galaxies at z ∼ 0 |journal=Monthly Notices of the Royal Astronomical Society |date=11 December 2009 |volume=400 |issue=3 |pages=1225–1240 |doi=10.1111/j.1365-2966.2009.15548.x|doi-access=free |arxiv=0908.3564 |bibcode=2009MNRAS.400.1225C }} The ring is elongated perpendicularly to the bar.

The optical disk is surrounded by a hydrogen envelope which extends to over 10 arcminutes from the nucleus, about two and half times more than the optical edge of the galaxy. The HI emission is about twice as strong at the west of the galaxy than the east but its western edge is sharper. The asymmetry could be the result of a past interaction with another galaxy.{{cite journal |last1=Kornreich |first1=David A. |last2=Haynes |first2=Martha P. |last3=Lovelace |first3=R. V. E. |last4=van Zee |first4=Liese |title=Departures From Axisymmetric Morphology and Dynamics in Spiral Galaxies |journal=The Astronomical Journal |date=July 2000 |volume=120 |issue=1 |pages=139–164 |doi=10.1086/301422|arxiv=astro-ph/0004113 |bibcode=2000AJ....120..139K }} Observations by the Arecibo Observatory revealed an HI cloud about 15 arcminutes northwest of the centre{{cite journal |last1=Duprie |first1=Kimberly |last2=Schneider |first2=Stephen E. |title=Neutral Hydrogen Around Early-Type Galaxies |journal=The Astronomical Journal |date=September 1996 |volume=112 |pages=937 |doi=10.1086/118067|bibcode=1996AJ....112..937D }} but it wasn't detected in observations by the Very Large Array.

NGC 5701 is according to A. M. Garcia a member of the NGC 5746 Group, also known as LGG 386.{{cite journal |last1=Garcia |first1=A. M. |title=General study of group membership. II. Determination of nearby groups. |journal=Astronomy and Astrophysics Supplement Series |date=1 July 1993 |volume=100 |pages=47–90 |url=https://cdsarc.cds.unistra.fr/ftp/J/A+AS/100/47/table2.dat |bibcode= 1993A&AS..100...47G |issn=0365-0138}} No companion galaxies are visible in hydrogen line or optical observations. UGC 9385, another member of the group, lies about 56 arcminutes to the west. The group is a member of the Virgo III Groups, a long chain of galaxies extending for about 40 million light years from the Virgo Cluster.{{cite web |title=The Virgo III Groups |url=http://www.atlasoftheuniverse.com/galgrps/viriii.html |website=www.atlasoftheuniverse.com |access-date=18 March 2025}}

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• [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=NGC%205701 NGC 5701 on SIMBAD]

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{{Virgo (constellation)}}

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Category:Barred lenticular galaxies

Category:Ring galaxies

Category:LINER galaxies

Category:Virgo (constellation)

5701

09436

52365

Category:Discoveries by William Herschel

Category:Astronomical objects discovered in 1786