NGC 1386 is aspiral galaxy located in the constellationEridanus. It is located at a distance of circa 53 millionlight years from Earth, which, given its apparent dimensions, means that NGC 1386 is about 50,000 light years across.[1] It is aSeyfert galaxy, the only one inFornax Cluster.
NGC 1386 was discovered byJohann Friedrich Julius Schmidt on January 19, 1865.[3] Julius Schmidt was then director of theNational Observatory of Athens and he was inspecting the Cape catalogue nebulae with a 6 ftrefractor. Along with NGC 1386, he also discovered the nearby galaxiesNGC 1381,NGC 1382,NGC 1389, andNGC 1428. The publication of their discovery was delayed by 10 years and was published in 1876 with the workÜber einige im Cape-Catalog fehlende Nebel.[4]
NGC 1386 is seen nearly edge-on and it has been classified both as a spiral and as alenticular galaxy. It features aspiral pattern with dust lanes. NoHII regions are visible in the images of the Carnegie Atlas of Galaxies,[5] however HII emission has been detected in the arms.[6] Dust features have also being observed at the central region of the galaxy.[7] Based on observations by theHerschel Space Telescope the total dust mass of NGC 1386 is estimated to be106.78M☉ and the stellar mass1010.5M☉.[8] The galaxy has two ring structures, with diameters of 0.5 and 1.67 arcminutes.[2]
The central region of NGC 1386 has three distinct kinematic components. The first has low velocity dispersion (approximately 90 km/s) and is identified as gas rotating in the galaxy disk. The second is observed in the inner 150 pc around the continuum peak and has two components, one redshifted and one blueshifted, which are identified as a bipolar outflow with an outflow rate of 0.1M☉ per year. The third element appears in velocity residual images and could be gas streaming inwards along the spiral. The galaxy disk has elevated emission at the location it intersects with the radiation from the AGN.[9]
Observations in 8.4 GHzradio waves by theVery Large Array reveal the presence of a linear radio feature extending to the south of the nucleus and a marginally detectable north extension. The brightest part of the south extension is 0".52 from the central source. Ionised gas is detected north and south of the nucleus in a position similar to the radio emission but a comparison with optical images shows no direct association.[11] A linear feature has also been observed byHubble Space Telescope in [O III] and [N II] +Hα with similar characteristics as the radio one. An emission plume extending for one arcsecond east-northeast of the nucleus was also observed.[7] No trace ofpolycyclic aromatic hydrocarbon (PAH) emission has been detected in mid-infrared observations of the central 20 pc of NGC 1386, while there is mildsilicate absorption, which may be associated with a dusttorus around the AGN.[12]
The Fornax Cluster byVLT Survey Telescope. NGC 1386 can be seen at lower centre left.
Observations byBeppoSAX andChandra X-Ray Observatory suggested that the nucleus of NGC 1386 is obscured by a Compton thick column, with high column density,[13][14] estimated to be(5±1)×1024 cm−2 as measured byNuSTAR.[15] The observations imply that the torus covers much of the nucleus.[16] The torus obscures much of the soft X-ray spectrum, but harder X-rays, as indicated by the Fe-Kα line manage to get through and be observed.[14] NGC 1386 has a corona with faint diffuse softX-ray emission that appears distorted at its outer parts.[17]
NGC 1386 has been found to host a cosmic watermaser.[18] It also features a HII region at the circumnuclear region.[19] The border between thenarrow-line region that isphotionisated by the AGN, and the surrounding HII regions is estimated to be at 6 arcseconds form the nucleus. That corresponds to 310 parsecs at the distance of NGC 1386.[20] A faint, inclined ring of emission extending up to 12 arcseconds from the nucleus can be seen in [N II] + Hα images, indicating also the presence of HII regions in the circumnuclear region.[7]
NGC 1386 is considered to be part of theFornax Cluster.[21] However, the redshift of NGC 1386 is smaller than that of the cluster and this has led to the assumption it is a foreground galaxy.[22] Makarov and Karachentsev grouped NGC 1386 in the NGC 1386 group, along withNGC 1389 andNGC 1396.[23]
^abComerón, S.; Salo, H.; Laurikainen, E.; Knapen, J. H.; Buta, R. J.; Herrera-Endoqui, M.; Laine, J.; Holwerda, B. W.; Sheth, K.; Regan, M. W.; Hinz, J. L.; Muñoz-Mateos, J. C.; Gil de Paz, A.; Menéndez-Delmestre, K.; Seibert, M.; Mizusawa, T.; Kim, T.; Erroz-Ferrer, S.; Gadotti, D. A.;Athanassoula, E.; Bosma, A.; Ho, L. C. (19 February 2014). "ARRAKIS: atlas of resonance rings as known in the S4G".Astronomy & Astrophysics.562: A121.arXiv:1312.0866.Bibcode:2014A&A...562A.121C.doi:10.1051/0004-6361/201321633.S2CID119295831.
^Sandage, A., Bedke, J. (1994),The Carnegie Atlas of Galaxies. Volume I, Carnegie Institution of Washington
^abWeaver, K. A.; Wilson, A. S.; Baldwin, J. A. (January 1991). "Kinematics and ionization of extended gas in active galaxies. VI - The Seyfert 2 galaxy NGC 1386".The Astrophysical Journal.366: 50.Bibcode:1991ApJ...366...50W.doi:10.1086/169539.
^abLena, D.; Robinson, A.; Storchi-Bergman, T.; Schnorr-Müller, A.; Seelig, T.; Riffel, R. A.; Nagar, N. M.; Couto, G. S.; Shadler, L. (9 June 2015). "The Complex Gas Kinematics in the Nucleus of the Seyfert 2 Galaxy NGC 1386: Rotation, Outflows, and Inflows".The Astrophysical Journal.806 (1): 84.arXiv:1504.05089.Bibcode:2015ApJ...806...84L.doi:10.1088/0004-637X/806/1/84.S2CID58937575.
^Maiolino, R.; Salvati, M.; Bassani, L.; Dadina, M.; della Ceca, R.; Matt, G.; Risaliti, G.; Zamorani, G. (1 October 1998). "Heavy obscuration in X-ray weak AGNs".Astronomy and Astrophysics.338:781–794.arXiv:astro-ph/9806055.Bibcode:1998A&A...338..781M.ISSN0004-6361.
^Masini, A.; Comastri, A.; Baloković, M.; Zaw, I.; Puccetti, S.; Ballantyne, D. R.; Bauer, F. E.; Boggs, S. E.; Brandt, W. N.; Brightman, M.; Christensen, F. E.; Craig, W. W.; Gandhi, P.; Hailey, C. J.; Harrison, F. A.; Koss, M. J.; Madejski, G.; Ricci, C.; Rivers, E.; Stern, D.; Zhang, W. W. (13 April 2016). "NuSTAR observations of water megamaser AGN".Astronomy & Astrophysics.589: A59.arXiv:1602.03185.Bibcode:2016A&A...589A..59M.doi:10.1051/0004-6361/201527689.S2CID43332114.
^Brightman, M.; Baloković, M.; Stern, D.; Arévalo, P.; Ballantyne, D. R.; Bauer, F. E.; Boggs, S. E.; Craig, W. W.; Christensen, F. E.; Comastri, A.; Fuerst, F.; Gandhi, P.; Hailey, C. J.; Harrison, F. A.; Hickox, R. C.; Koss, M.; LaMassa, S.; Puccetti, S.; Rivers, E.; Vasudevan, R.; Walton, D. J.; Zhang, W. W. (19 May 2015). "Determining the Covering Factor of Compton-thick Active Galactic Nuclei with NuSTAR".The Astrophysical Journal.805 (1): 41.arXiv:1502.07353.Bibcode:2015ApJ...805...41B.doi:10.1088/0004-637X/805/1/41.S2CID7842878.
^Braatz, J.; Greenhill, L.; Moran, J.; Wilson, A.; Herrnstein, J. (1 December 1997). "A VLBA Map of the H_2O Maser in the Nucleus of Seyfert 2 Galaxy NGC 1386".American Astronomical Society Meeting Abstracts.191: 104.02.Bibcode:1997AAS...19110402B.
^Storchi-Bergmann, Thaisa; Rodriguez-Ardila, Alberto; Schmitt, Henrique R.; Wilson, Andrew S.; Baldwin, Jack A. (20 November 1996). "Circumnuclear Star Formation in Active Galaxies".The Astrophysical Journal.472 (1):83–101.Bibcode:1996ApJ...472...83S.doi:10.1086/178043.hdl:10183/108769.S2CID123352311.
^Sarzi, M.; Iodice, E.; Coccato, L.; Corsini, E. M.; de Zeeuw, P. T.; Falcón-Barroso, J.; Gadotti, D. A.; Lyubenova, M.; McDermid, R. M.; de Ven, G. van; Fahrion, K.; Pizzella, A.; Zhu, L. (28 August 2018). "Fornax3D project: Overall goals, galaxy sample, MUSE data analysis, and initial results".Astronomy & Astrophysics.616: A121.arXiv:1804.06795.Bibcode:2018A&A...616A.121S.doi:10.1051/0004-6361/201833137.S2CID118855983.
^Rossa, J.; Dietrich, M.; Wagner, S.J. (October 2000). "Kinematics and morphology of the Narrow-Line Region in the Seyfert galaxy NGC1386".Astronomy and Astrophysics.362:501–508.arXiv:astro-ph/0008269.Bibcode:2000A&A...362..501R.
