NGC 1371,UGCA 79, ESO 482- G 010, AM 0332-250,MCG -04-09-029, IRAS F03328-2505,PGC 13255
NGC 1367 orNGC 1371 is aspiral galaxy in the constellationFornax. The galaxy lies about 75 millionlight years away from Earth, which means, given its apparent dimensions, that NGC 1367 is approximately 130,000 light years across.[1] It was discovered byWilliam Herschel on November 17, 1784, and independently byOrmond Stone in 1886.[3] It is a member of theEridanus Cluster.
The galaxy is seen inclined, at an angle of 47.5°.[4] It has a bright bulge featuring a weak bar with ansae at its ends from where low surface brightness arms with no obvious knots emerge.[5]H-alpha imaging shows the presence ofHII regions in the arms and a circumnuclear ring, surrounding a central source.[6] The galaxy has a faint outerring.[5] Star formation takes place in the outer arms of the galaxy while the bulge does not appear to be forming stars at a significant rate.[7]
The galaxy has a disk with X-ray emission, measuring 31 by 16 arcseconds, and faint diffuse X-ray emission extending beyond it. The inner disk emission could be due tosupernova remnants,X-ray binary stars and strong stellar winds. Three individual X-ray sources are nearly coincident with individual HII regions.[8] The galaxy has an extended hydrogen disk, with a diameter of 22.3 arcminutes.[7] The total hydrogen I mass of the galaxy is estimated to be109.95M☉.[4]
When observed in radiowaves a kpc-scale linearjet like structure is revealed and a bright radio source. Observations by theAustralian Square Kilometre Array Pathfinder reveal doubleradio lobes and jets. The radio jets of this galaxy have half the extent of the inner stellar disk, lie slightly offset from the bar, and coincide with a hole inhydrogen emission.[7] The radio emission excess indicates that the nucleus of the galaxy isactive,[6] belonging to the same class asNGC 3079 andCircinus Galaxy.[7] The flux of the nuclear source observed by theChandra X-ray Observatory is consistent with a low luminosity AGN, like aSeyfert galaxy orLINER.[8]
In the centre of the galaxy is predicted to lie asupermassive black hole whose mass is estimated to be between 0.47 and 4.7 millionsolar masses, based on the spiral arm pitch angle,[9] or 25 million solar masses based on theM–sigma relation.[10]
One supernova has been observed in NGC 1367,SN 2005ke. The supernova was discovered on 13 November 2005 by M. Baek, R. R. Prasad, and W. Li using theKatzman Automatic Imaging Telescope. The supernova had an apparent magnitude of 17.2 upon discovery.[11] Its spectrum on 16 November indicated it was an underluminousType Ia supernova before maximum.[12] Observations in X-rays and ultraviolet indicate that the supernova shock wave interacted with the circumstellar medium, consisting of material deposited by the stellar winds of the progenitor system.[13]
^abEskridge, Paul B.; Frogel, Jay A.; Pogge, Richard W.; Quillen, Alice C.; Berlind, Andreas A.; Davies, Roger L.; DePoy, D. L.; Gilbert, Karoline M.; Houdashelt, Mark L.; Kuchinski, Leslie E.; Ramirez, Solange V.; Sellgren, K.; Stutz, Amelia; Terndrup, Donald M.; Tiede, Glenn P. (November 2002). "Near-Infrared and Optical Morphology of Spiral Galaxies".The Astrophysical Journal Supplement Series.143 (1):73–111.arXiv:astro-ph/0206320.Bibcode:2002ApJS..143...73E.doi:10.1086/342340.
^abcdGrundy, J. A.; Wong, O. I.; Lee-Waddell, K.; Seymour, N.; For, B.-Q.; Murugeshan, C.; Koribalski, B. S.; Madrid, J. P.; Rhee, J.; Westmeier, T. (2023). "WALLABY pre-pilot survey: Radio continuum properties of the Eridanus supergroup".Publications of the Astronomical Society of Australia.40.arXiv:2303.00626.Bibcode:2023PASA...40...12G.doi:10.1017/pasa.2023.11.
^abHughes, John P.; Chugai, Nikolai; Chevalier, Roger; Lundqvist, Peter; Schlegel, Eric (December 2007). "Chandra Observations of Type Ia Supernovae: Upper Limits to the X-Ray Flux of SN 2002bo, SN 2002ic, SN 2005gj, and SN 2005ke".The Astrophysical Journal.670 (2):1260–1274.arXiv:0710.3190.Bibcode:2007ApJ...670.1260H.doi:10.1086/522113.
^Davis, Benjamin L.; Berrier, Joel C.; Johns, Lucas; Shields, Douglas W.; Hartley, Matthew T.; Kennefick, Daniel; Kennefick, Julia; Seigar, Marc S.; Lacy, Claud H. S. (20 June 2014). "The Black Hole Mass Function Derived from Local Spiral Galaxies".The Astrophysical Journal.789 (2): 124.arXiv:1405.5876.Bibcode:2014ApJ...789..124D.doi:10.1088/0004-637X/789/2/124.
^Cisternas, Mauricio; Gadotti, Dimitri A.; Knapen, Johan H.; Kim, Taehyun; Díaz-García, Simón; Laurikainen, Eija; Salo, Heikki; González-Martín, Omaira; Ho, Luis C.; Elmegreen, Bruce G.; Zaritsky, Dennis; Sheth, Kartik; Athanassoula, E.; Bosma, Albert; Comerón, Sébastien; Erroz-Ferrer, Santiago; Gil de Paz, Armando; Hinz, Joannah L.; Holwerda, Benne W.; Laine, Jarkko; Meidt, Sharon; Menéndez-Delmestre, Karín; Mizusawa, Trisha; Muñoz-Mateos, Juan Carlos; Regan, Michael W.; Seibert, Mark (25 September 2013). "X-RAY NUCLEAR ACTIVITY IN S4G BARRED GALAXIES: NO LINK BETWEEN BAR STRENGTH AND CO-OCCURRENT SUPERMASSIVE BLACK HOLE FUELING".The Astrophysical Journal.776 (1): 50.arXiv:1307.7709.Bibcode:2013ApJ...776...50C.doi:10.1088/0004-637X/776/1/50.
^Patat, F.; Baade, D.; Wang, L.; Taubenberger, S.; Wheeler, J. C. (1 November 2005)."Supernova 2005ke in NGC 1371".International Astronomical Union Circular (8631): 1.ISSN0081-0304.
^Immler, S.; Brown, P. J.; Milne, P.; The, L.-S.; Petre, R.; Gehrels, N.; Burrows, D. N.; Nousek, J. A.; Williams, C. L.; Pian, E.; Mazzali, P. A.; Nomoto, K.; Chevalier, R. A.; Mangano, V.; Holland, S. T.; Roming, P. W. A.; Greiner, J.; Pooley, D. (10 September 2006). "X-Ray Observations of Type Ia Supernovae with Swift : Evidence of Circumstellar Interaction for SN 2005ke".The Astrophysical Journal.648 (2):L119–L122.arXiv:astro-ph/0607620.Bibcode:2006ApJ...648L.119I.doi:10.1086/507947.
