Markarian 273
{{short description|Galaxy in the constellation of Ursa Major}}
{{Infobox galaxy
| name = Markarian 273
| image = 250px
| caption = Mrk 273 by the Hubble Space Telescope
| epoch = J2000
| type = Pec {{cite web
| title=NASA/IPAC Extragalactic Database
| work=Results for MRK 273
| url=http://ned.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=MRK+273
| access-date=2023-05-06 }}
| h_radial_v = 11,194 ± 2 km/s
| appmag_v = 14.8
| size_v = 0.72{{prime}} × 0.40{{prime}}
| constellation name = Ursa Major
| notes = Ultraluminous infrared galaxy, Seyfert galaxy
| names = UGC 8696, VV 851, I Zw 071, MCG +09-23-004, PGC 48711
}}
Markarian 273 is a galaxy merger located in the constellation Ursa Major. It is located at a distance of about 500 million light years from Earth, which, given its apparent dimensions, means that Markarian 273 is about 130,000 light years across. It is an ultraluminous infrared galaxy and a Seyfert galaxy.
Characteristics
Markarian 273 is a galaxy merger, the result of two or more galaxies colliding. When observed in mid infrared, two nuclei are visible, with a projected separation of about 0.75 kiloparsec.{{cite journal |last1=Liu |first1=Weizhe |last2=Veilleux |first2=Sylvain |last3=Iwasawa |first3=Kazushi |last4=Rupke |first4=David S. N. |last5=Teng |first5=Stacy |last6=U |first6=Vivian |last7=Tombesi |first7=Francesco |last8=Sanders |first8=David |last9=Max |first9=Claire E. |last10=Meléndez |first10=Marcio |title=Elliptical Galaxy in the Making: The Dual Active Galactic Nuclei and Metal-enriched Halo of Mrk 273 |journal=The Astrophysical Journal |date=8 February 2019 |volume=872 |issue=1 |pages=39 |doi=10.3847/1538-4357/aafdfc|arxiv=1901.04118 |bibcode=2019ApJ...872...39L |doi-access=free }} The southwest nucleus is known to be active, due its X-ray emission,{{cite journal |last1=Iwasawa |first1=K. |last2=Mazzarella |first2=J. M. |last3=Surace |first3=J. A. |last4=Sanders |first4=D. B. |last5=Armus |first5=L. |last6=Evans |first6=A. S. |last7=Howell |first7=J. H. |last8=Komossa |first8=S. |last9=Petric |first9=A. |last10=Teng |first10=S. H. |last11=U |first11=V. |last12=Veilleux |first12=S. |title=The location of an active nucleus and a shadow of a tidal tail in the ULIRG Mrk 273 |journal=Astronomy & Astrophysics |date=April 2011 |volume=528 |pages=A137 |doi=10.1051/0004-6361/201015872|arxiv=1101.3659 |bibcode=2011A&A...528A.137I |doi-access=free }} while the northeast nucleus too displays a heavily absorbed X-ray spectrum, indicating that is also active. The optical emission of the southwest nucleus corresponds to a type II Seyfert galaxy while the north one of a LINER.{{cite journal |last1=Colina |first1=Luis |last2=Arribas |first2=Santiago |last3=Borne |first3=Kirk D. |title=Integral Field Spectroscopy of Markarian 273: Mapping High-Velocity Gas Flows and an Off-Nucleus Seyfert 2 Nebula |journal=The Astrophysical Journal |date=10 December 1999 |volume=527 |issue=1 |pages=L13–L16 |doi=10.1086/312389|pmid=10566988 |arxiv=astro-ph/9910344 |bibcode=1999ApJ...527L..13C |hdl=10261/199205 |s2cid=27436431 |hdl-access=free }} A third component in the nuclear region is visible at the southeast in the radiowaves and could be a star cluster.
The galaxy experiences a starburst, with a star formation rate of 139 {{solar mass}} per year.{{cite journal |last1=Cicone |first1=C. |last2=Maiolino |first2=R. |last3=Sturm |first3=E. |last4=Graciá-Carpio |first4=J. |last5=Feruglio |first5=C. |last6=Neri |first6=R. |last7=Aalto |first7=S. |last8=Davies |first8=R. |last9=Fiore |first9=F. |last10=Fischer |first10=J. |last11=García-Burillo |first11=S. |last12=González-Alfonso |first12=E. |last13=Hailey-Dunsheath |first13=S. |last14=Piconcelli |first14=E. |last15=Veilleux |first15=S. |title=Massive molecular outflows and evidence for AGN feedback from CO observations |journal=Astronomy & Astrophysics |date=February 2014 |volume=562 |pages=A21 |doi=10.1051/0004-6361/201322464|arxiv=1311.2595 |bibcode=2014A&A...562A..21C |doi-access=free }} This activity makes the galaxy shine bright in the infrared and it is categorised as ultra-luminous infrared galaxy, with total infrared luminosity of the galaxy is estimated to be {{val|e=12.1|ul=L_solar}}.{{cite journal |last1=Kim |first1=D.-C. |last2=Veilleux |first2=S. |last3=Sanders |first3=D. B. |title=Optical and Near-Infrared Imaging of the IRAS 1 Jy Sample of Ultraluminous Infrared Galaxies. I. The Atlas |journal=The Astrophysical Journal Supplement Series |date=December 2002 |volume=143 |issue=2 |pages=277–314 |doi=10.1086/343843|arxiv=astro-ph/0207373 |bibcode=2002ApJS..143..277K |doi-access=free }} The startburst takes place in a rotating disk with a radius 120 pc and a total mass of {{val|2.6|e=9|u=M_solar}} which surrounds the north nucleus.{{cite journal |last1=Downes |first1=D. |last2=Solomon |first2=P. M. |title=Rotating Nuclear Rings and Extreme Starbursts in Ultraluminous Galaxies |journal=The Astrophysical Journal |date=10 November 1998 |volume=507 |issue=2 |pages=615–654 |doi=10.1086/306339|arxiv=astro-ph/9806377 |bibcode=1998ApJ...507..615D |doi-access=free }} It has been suggested that this is the location of compact luminous supernovae remnants and radio supernovae.{{cite journal |last1=Bondi |first1=M. |last2=Pérez-Torres |first2=M-A. |last3=Dallacasa |first3=D. |last4=Muxlow |first4=T. W. B. |title=A supernova factory in Mrk 273? |journal=Monthly Notices of the Royal Astronomical Society |date=September 2005 |volume=361 |issue=2 |pages=748–752 |doi=10.1111/j.1365-2966.2005.09206.x|arxiv=astro-ph/0505370 |bibcode=2005MNRAS.361..748B |doi-access=free }} The startburst is fed by large amounts of cold molecular gas. The gas has complex kinematics due to the presence of outflows. A kiloparsec scale outflow is visible towards the north in CO imaging, with the flow rate of 600 {{solar mass}} per year. The outflows reach about 5 kpc from the nucleus.{{cite journal |last1=Leung |first1=Gene C. K. |last2=Coil |first2=Alison L.|author2-link=Alison Coil |last3=Rupke |first3=David S. N. |last4=Perrotta |first4=Serena |title=KCWI Observations of the Extended Nebulae in Mrk 273 |journal=The Astrophysical Journal |date=1 June 2021 |volume=914 |issue=1 |pages=17 |doi=10.3847/1538-4357/abf4da|arxiv=2011.09587 |bibcode=2021ApJ...914...17L |doi-access=free }} There is also evidence of a bipolar superbubble.{{cite journal |last1=Rupke |first1=David S. N. |last2=Veilleux |first2=Sylvain |title=The Multiphase Structure and Power Sources of Galactic Winds in Major Mergers |journal=The Astrophysical Journal |date=16 April 2013 |volume=768 |issue=1 |pages=75 |doi=10.1088/0004-637X/768/1/75|arxiv=1303.6866 |bibcode=2013ApJ...768...75R |s2cid=118390059 }}
The merger has a tidal tail extending southwards for 40 kiloparsecs, that is seen edge-on. Also south of the galaxy lies a giant X-ray nebula, measuring 40 by 40 kiloparsecs in size, that isn't closely related with the tidal tail. The gas temperature of the nebula is estimated to be 7 million K, possibly heated by galactic outflows. Filaments and clumps of ionised gas visible in OIII are extending about 23 kpc to the east.{{cite journal |last1=Rodríguez Zaurín |first1=J. |last2=Tadhunter |first2=C. N. |last3=Rupke |first3=D. S. N. |last4=Veilleux |first4=S. |last5=Spoon |first5=H. W. W. |last6=Chiaberge |first6=M. |last7=Ramos Almeida |first7=C. |last8=Batcheldor |first8=D. |last9=Sparks |first9=W. B. |title=Extended warm gas in the ULIRG Mrk273: Galactic outflows and tidal debris |journal=Astronomy & Astrophysics |date=November 2014 |volume=571 |pages=A57 |doi=10.1051/0004-6361/201423540|arxiv=1407.6301 |bibcode=2014A&A...571A..57R |s2cid=59132144 }} A warm gas ionised halo extends about 45 kpc from the nucleus, and is probably tidal debris from the merger.{{cite journal |last1=Spence |first1=R. A. W. |last2=Zaurín |first2=J. Rodríguez |last3=Tadhunter |first3=C. N. |last4=Rose |first4=M. |last5=Cabrera-Lavers |first5=A. |last6=Spoon |first6=H. |last7=Muñoz-Tuñón |first7=C. |title=No evidence for large-scale outflows in the extended ionized halo of ULIRG Mrk273 |journal=Monthly Notices of the Royal Astronomical Society: Letters |date=11 June 2016 |volume=459 |issue=1 |pages=L16–L20 |doi=10.1093/mnrasl/slw033|doi-access=free |arxiv=1603.00488 }} When observed in radiowaves the galaxy has two large plumes, one to the south, extending to about 100 kpc, and one dimmer to the north, extending to about 190 kpc.{{cite journal |last1=Kukreti |first1=P. |last2=Morganti |first2=R. |author2-link=Raffaella Morganti |last3=Bondi |first3=M. |last4=Oosterloo |first4=T. |last5=Tadhunter |first5=C. |last6=Morabito |first6=L. K. |last7=Adams |first7=E. A. K. |last8=Adebahr |first8=B. |last9=de Blok |first9=W. J. G. |last10=de Gasperin |first10=F. |last11=Drabent |first11=A. |last12=Hess |first12=K. M. |last13=Ivashina |first13=M. V. |author-link13=Marianna Ivashina |last14=Kutkin |first14=A. |last15=Mika |first15=á. M. |date=August 2022 |title=Seeing the forest and the trees: A radio investigation of the ULIRG Mrk 273 |journal=Astronomy & Astrophysics |volume=664 |pages=A25 |arxiv=2206.02847 |bibcode=2022A&A...664A..25K |doi=10.1051/0004-6361/202243174 |doi-access=free |last16=Oostrum |first16=L. C. |last17=Shimwell |first17=T. W. |last18=van der Hulst |first18=J. M. |last19=van Leeuwen |first19=J. |last20=van Weeren |first20=R. J. |last21=Vohl |first21=D. |last22=Ziemke |first22=J.}}
See also
References
{{Reflist}}
External links
{{wikiSky}}
- [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=MRK%20273 Markarian 273 on SIMBAD]
{{Ursa Major}}
{{DEFAULTSORT:Markarian 273}}