Markarian 463
{{Short description|Galaxy in the constellation of Boötes}}
{{Infobox galaxy|name=Markarian 463|epoch=J2000|constellation name=Boötes|ra={{RA|13|56|02.87}}|dec={{DEC|+18|22|19.48}}|z=0.050802|h_radial_v=15,230 km/s|dist_ly=706 Mly (216.5 Mpc)|appmag_v=0.079|appmag_b=0.104|type=Merger; Sy1, Sy2|notes=luminous infrared galaxy, double active galactic nucleus, seyfert galaxy|names=UGC 8850, PGC 49538, KUG 1353+186, MCG +03-36-005, IRAS 13536+1836, TXS 1353+186|image=File:SDSS image of Markarian 463.jpg|caption=Mrk 463 by SDSS}}
Markarian 463 (Mrk 463) known as UGC 8850, is a galaxy merger located in the constellation Boötes. It is located 706 million light years from Earth.{{Cite web |title=Your NED Search Results |url=https://ned.ipac.caltech.edu/cgi-bin/objsearch?extend=no&hconst=73&omegam=0.27&omegav=0.73&corr_z=1&out_csys=Equatorial&out_equinox=J2000.0&obj_sort=RA+or+Longitude&of=pre_text&zv_breaker=30000.0&list_limit=5&img_stamp=YES&objname=Mrk%20463 |access-date=2024-09-19 |website=ned.ipac.caltech.edu}} It is classified a double nucleus Seyfert galaxy.{{Cite journal |last1=Rafanelli |first1=P. |last2=di Serego Alighieri |first2=S. |date=1986-01-01 |title=PCD spectroscopy of Mkn 463, a double nucleus Seyfert-2 galaxy. |journal=Structure and Evolution of Active Galactic Nuclei |url=https://ui.adsabs.harvard.edu/abs/1986ASSL..121..689R/abstract |volume=121 |pages=689–692 |doi=10.1007/978-90-277-2155-6_76|doi-broken-date=1 November 2024 |bibcode=1986ASSL..121..689R }}{{Cite journal |last1=Rafanelli |first1=Piero |last2=Marziani |first2=Paolo |date=1990-11-01 |title=The double nucleus galaxies Mkn 423 and Mkn 739 |url=https://ntrs.nasa.gov/citations/19910007578 |journal=NASA, Marshall Space Flight Center, Paired and Interacting Galaxies: International Astronomical Union Colloquium No. 124 |volume=3098 |issue=124 |page=225 |bibcode=1990NASCP3098..225R |language=en}}
Characteristics
Markarian 463 is a late stage galaxy merger, a product of two gas-rich spiral galaxies colliding with one another. According to optical and near-infrared observations, the galaxy is shown to have a complex morphology with star forming clumps and curved tidal tails.{{Cite journal |last1=Treister |first1=Ezequiel |last2=Privon |first2=George C. |last3=Sartori |first3=Lia F. |last4=Nagar |first4=Neil |last5=Bauer |first5=Franz E. |last6=Schawinski |first6=Kevin |last7=Messias |first7=Hugo |last8=Ricci |first8=Claudio |last9=U |first9=Vivian |last10=Casey |first10=Caitlin |last11=Comerford |first11=Julia M. |last12=Muller-Sanchez |first12=Francisco |last13=Evans |first13=Aaron S. |last14=Finlez |first14=Carolina |last15=Koss |first15=Michael |date=2018-02-15 |title=Optical, Near-IR, and Sub-mm IFU Observations of the Nearby Dual Active Galactic Nuclei MRK 463 |journal=The Astrophysical Journal |volume=854 |issue=2 |pages=83 |doi=10.3847/1538-4357/aaa963 |doi-access=free |arxiv=1801.06190 |bibcode=2018ApJ...854...83T |issn=0004-637X}} It has a luminosity of LIR (8–1000μm) = 1011.8 LΘ making it a luminous infrared galaxy.{{Cite journal |last1=Imanishi |first1=Masatoshi |last2=Saito |first2=Yuriko |date=2013-12-13 |title=SUBARU ADAPTIVE-OPTICS HIGH-SPATIAL-RESOLUTION INFRAREDK- ANDL′-BAND IMAGING SEARCH FOR DEEPLY BURIED DUAL AGNs IN MERGING GALAXIES |url=http://dx.doi.org/10.1088/0004-637x/780/1/106 |journal=The Astrophysical Journal |volume=780 |issue=1 |pages=106 |doi=10.1088/0004-637x/780/1/106 |issn=0004-637X|arxiv=1312.2031 }} It contains a compact radio flux in either linear or elongated structure.{{Cite journal |last1=Neff |first1=S. G. |last2=Ulvestad |first2=J. S. |date=1988-09-01 |title=Compact Radio Cores in Three Seyfert Galaxies: High-Resolution Studies of MKN 3, MKN 231, and MKN 463 |url=https://ui.adsabs.harvard.edu/abs/1988AJ.....96..841N/abstract |journal=The Astronomical Journal |volume=96 |pages=841 |doi=10.1086/114850 |bibcode=1988AJ.....96..841N |issn=0004-6256}} Using spectra captured by the Infrared Spectrograph installed on Spitzer Space Telescope, emission lines are detected in Markarian 463 hinting a warm supply of molecular gas.{{Cite journal |last1=Armus |first1=L. |last2=Charmandaris |first2=V. |last3=Spoon |first3=H. W. W. |last4=Houck |first4=J. R. |last5=Soifer |first5=B. T. |last6=Brandl |first6=B. R. |last7=Appleton |first7=P. N. |last8=Teplitz |first8=H. I. |last9=Higdon |first9=S. J. U. |last10=Weedman |first10=D. W. |last11=Devost |first11=D. |last12=Morris |first12=P. W. |last13=Uchida |first13=K. I. |last14=Cleve |first14=J. van |last15=Barry |first15=D. J. |date=2004-09-01 |title=Observations of Ultraluminous Infrared Galaxies with the Infrared Spectrograph (IRS) on the Spitzer Space Telescope: Early Results on Markarian 1014, Markarian 463, and UGC 5101* |url=https://iopscience.iop.org/article/10.1086/422915 |journal=The Astrophysical Journal Supplement Series |language=en |volume=154 |issue=1 |pages=178 |doi=10.1086/422915 |arxiv=astro-ph/0406179 |bibcode=2004ApJS..154..178A |issn=0067-0049}}
A broadband X-ray spectral analysis revealed two obscured nuclei designated as Markarian 463W and Markarian 463E, with an estimated projected separation of ~ 3.8 kiloparsec.{{Cite journal |last1=Yamada |first1=Satoshi |last2=Ueda |first2=Yoshihiro |last3=Oda |first3=Saeko |last4=Tanimoto |first4=Atsushi |last5=Imanishi |first5=Masatoshi |last6=Terashima |first6=Yuichi |last7=Ricci |first7=Claudio |date=2018-05-10 |title=Broadband X-Ray Spectral Analysis of the Double-nucleus Luminous Infrared Galaxy Mrk 463 |journal=The Astrophysical Journal |volume=858 |issue=2 |pages=106 |doi=10.3847/1538-4357/aabacb |doi-access=free |arxiv=1803.11223 |bibcode=2018ApJ...858..106Y |issn=0004-637X}} This finding makes the galaxy a dual active galactic nucleus{{Cite journal |last1=Das |first1=Mousumi |last2=Rubinur |first2=Khatun |last3=Kharb |first3=Preeti |last4=Varghese |first4=Ashlin |last5=Novakkuni |first5=Navyasree |last6=James |first6=Atul |date=2018-04-01 |title=Dual Active Galactic Nuclei in Nearby Galaxies |url=https://ui.adsabs.harvard.edu/abs/2018BSRSL..87..299D/abstract |journal=Bulletin de la Société Royale des Sciences de Liège |volume=87 |pages=299–306 |arxiv=1708.01185|bibcode=2018BSRSL..87..299D }} and is the third closest physical pair known after NGC 6240 and NGC 3758. The two nuclei has a luminosity of L2–10keV = {{val|1.5|e=43}} and {{val|3.8|e= 42|u=erg cm−2 s−1}}.{{Cite journal |last1=Bianchi |first1=Stefano |last2=Chiaberge |first2=Marco |last3=Piconcelli |first3=Enrico |last4=Guainazzi |first4=Matteo |last5=Matt |first5=Giorgio |date=2008-05-01 |title=Chandra unveils a binary active galactic nucleus in Mrk 463 |journal=Monthly Notices of the Royal Astronomical Society |volume=386 |issue=1 |pages=105–110 |doi=10.1111/j.1365-2966.2008.13078.x |doi-access=free |arxiv=0802.0825 |bibcode=2008MNRAS.386..105B |issn=0035-8711}} Both are active and are expected to drawn close to each other over timescales of 108 years.
The western nucleus has a moderate radio luminosity equivalent of an extremely luminous starburst galaxy or a Seyfert galaxy through imaging detections at 6 and 20 centimeters.{{Cite journal |last1=Mazzarella |first1=J. M. |last2=Gaume |first2=R. A. |last3=Soifer |first3=B. T. |last4=Graham |first4=J. R. |last5=Neugebauer |first5=G. |last6=Matthews |first6=K. |date=1991-10-01 |title=The dust enshrouded quasar in the ultraluminous galaxy Markarian 463: radio, near-infrared, and optical imaging. |url=https://authors.library.caltech.edu/records/5sfzm-rfv72/files/1991AJ____102_1241M.pdf?download=1 |journal=The Astronomical Journal |volume=102 |pages=1241–1252 |doi=10.1086/115950 |bibcode=1991AJ....102.1241M |issn=0004-6256}} The eastern nucleus however, is much brighter compared to the western nucleus, and is classified a type II Seyfert galaxy. It is found offset from its peak flux and shows polarized conical wind. With a half-opening angle of ~ 15 degrees, its wind displays three mass ejection periods.{{Citation |last1=Barnouin |first1=Thibault |title=Forgotten treasures in the HST/FOC UV imaging polarimetric archives of active galactic nuclei |date=2024-06-01 |url=https://ui.adsabs.harvard.edu/abs/2024arXiv240613021B/abstract |access-date=2024-09-19 |arxiv=2406.13021 |last2=Marin |first2=Frédéric |last3=Lopez-Rodriguez |first3=Enrique|journal=Astronomy & Astrophysics |volume=692 |pages=A178 |doi=10.1051/0004-6361/202451105 }} Using infrared spectroscopy, the eastern nucleus hosts a hidden Seyfert 1 nucleus located southwards but not co-spatial.{{Cite journal |last1=Kukula |first1=Marek J. |last2=Ghosh |first2=Tapasi |last3=Pedlar |first3=Alan |last4=Schilizzi |first4=Richard T. |date=1999-06-10 |title=Parsec-Scale Radio Structures in the Nuclei of Four Seyfert Galaxies |url=http://dx.doi.org/10.1086/307254 |journal=The Astrophysical Journal |volume=518 |issue=1 |pages=117–128 |doi=10.1086/307254 |arxiv=astro-ph/9904186 |bibcode=1999ApJ...518..117K |issn=0004-637X}}
According to Chandra X-ray data, the supermassive black hole in the nucleus of Markarian 463E has a much higher accretion rate of ~ 5x. It is also associated with emission and continuum lines. It is also shown it is older compared the nucleus of Markarian 463W, given the northern outflowing cloud and southern emission region appears generally aligned with the biconical gradient. An ALMA 12CO (2–1) observation also finds the two nuclei have molecular gas reservoirs estimated of ~ 109 MΘ and ~ 5 × 108 MΘ respectively. Given enough molecular gas provided, it is enough to feed both black holes in the galaxy.
Markarian 463 has an optical jet originating from the Seyfert nucleus according to Hubble Space Telescope imaging. The jet is found to reach the end at the radio source found 1.2 arcsecs away, and is measured 0.84 arcsecs with a position angle of 182 degrees.{{Cite journal |last1=Uomoto |first1=A. |last2=Caganoff |first2=S. |last3=Ford |first3=H. C. |last4=Rosenblatt |first4=E. I. |last5=Evans |first5=I. N. |last6=Cohen |first6=R. D. |date=1992-05-01 |title=The Optical Jet in Markarian 463 |journal=American Astronomical Society Meeting Abstracts #180 |url=https://ui.adsabs.harvard.edu/abs/1992AAS...180.1603U/abstract |volume=180 |pages=16.03|bibcode=1992AAS...180.1603U }}
Part of the galaxy shows emission due to oxygen, first identified with Hubble. This was interpreted as a possible extended emission-line region (EELR).{{Cite journal |last1=Keel |first1=William C. |last2=Chojnowski |first2=S. Drew |last3=Bennert |first3=Vardha N. |last4=Schawinski |first4=Kevin |last5=Lintott |first5=Chris J. |last6=Lynn |first6=Stuart |last7=Pancoast |first7=Anna |last8=Harris |first8=Chelsea |last9=Nierenberg |first9=A. M. |last10=Sonnenfeld |first10=Alessandro |last11=Proctor |first11=Richard |date=2012-02-01 |title=The Galaxy Zoo survey for giant AGN-ionized clouds: past and present black hole accretion events |journal=Monthly Notices of the Royal Astronomical Society |volume=420 |issue=1 |pages=878–900 |arxiv=1110.6921 |bibcode=2012MNRAS.420..878K |doi=10.1111/j.1365-2966.2011.20101.x |issn=0035-8711 |doi-access=free}}
Gallery
File:Mrk 463 Hubble WFPC2.jpg|Hubble image of Mrk 463, with oxygen being green
File:Mrk 463 MUSE.jpg|VLT MUSE image of Mrk 463, with H-alpha being orange and oxygen being green
File:Mrk 463 legacy dr10.jpg|Mrk 463 in wide view with legacy surveys, showing the tidal arms
References
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{{Boötes}}
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Category:Luminous infrared galaxies