NGC 1386

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NGC 1386
NGC 1386 -HST06419 02R791GB658n.png
NGC 1386 by the Hubble Space Telescope
Observation data (J2000 epoch)
Constellation Eridanus
Right ascension 03h 36m 46.2s [1]
Declination −35° 59′ 58″ [1]
Redshift 0.002895 ± 0.000017 [1]
Heliocentric radial velocity 868 ± 5 km/s [1]
Distance 52.6 ± 2.3 Mly (16.2 ± 0.7 Mpc) [1]
Group or cluster Fornax cluster
Apparent magnitude  (V)11.2
Characteristics
Type (R′)SA(r)0/a [2]
Apparent size  (V)3.4′ × 1.3′ [1]
Notable featuresSeyfert galaxy
Other designations
ESO 358- G035, FCC 179, MCG -06-09-005, PGC 13333 [1]

NGC 1386 is a spiral galaxy located in the constellation Eridanus. It is located at a distance of circa 53 million light years from Earth, which, given its apparent dimensions, means that NGC 1386 is about 50,000 light years across. [1] It is a Seyfert galaxy, the only one in Fornax Cluster.

Contents

Observation history

NGC 1386 was discovered by Johann Friedrich Julius Schmidt on January 19, 1865. [3] Julius Schmidt was then director of the National Observatory of Athens and he was inspecting the Cape catalogue nebulae with a 6 ft refractor. Along with NGC 1386, he also discovered the nearby galaxies NGC 1381, NGC 1382, NGC 1389, and NGC 1428. The publication of their discovery was delayed by 10 years and was published in 1876 with the work Über einige im Cape-Catalog fehlende Nebel. [4]

Characteristics

NGC 1386 is seen nearly edge-on and it has been classified both as a spiral and as a lenticular galaxy. It features a spiral pattern with dust lanes. No HII 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 the Herschel Space Telescope the total dust mass of NGC 1386 is estimated to be 106.78  M☉ and the stellar mass 1010.5  M☉ . [8] The galaxy has two ring structures, with diameters of 0.5 and 1.67 arcminutes. [2]

Active galactic nucleus

NGC 1386 has an active galactic nucleus (AGN) that has been categorised as a type 2 Seyfert galaxy. [6] It is one of the nearest Seyfert galaxies. The source of nuclear activity in galaxies is suggested to be material accretion around a supermassive black hole in the galactic centre. [9] The black hole in the centre of NGC 1386 is estimated to be 2.6×107  M☉ based on stellar velocity dispersion. [10]

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 0.1 M☉ 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 GHz radio waves by the Very 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 by Hubble 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 of polycyclic aromatic hydrocarbon (PAH) emission has been detected in mid-infrared observations of the central 20 pc of NGC 1386, while there is mild silicate absorption, which may be associated with a dust torus around the AGN. [12]

The Fornax Cluster by VLT Survey Telescope. NGC 1386 can be seen at lower centre left. VST image of the Fornax Galaxy Cluster.jpg
The Fornax Cluster by VLT Survey Telescope. NGC 1386 can be seen at lower centre left.

Observations by BeppoSAX and Chandra 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 by NuSTAR. [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 soft X-ray emission that appears distorted at its outer parts. [17]

NGC 1386 has been found to host a cosmic water maser. [18] It also features a HII region at the circumnuclear region. [19] The border between the narrow-line region that is photionisated 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]

Nearby galaxies

NGC 1386 is considered to be part of the Fornax 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 with NGC 1389 and NGC 1396. [23]

See also

Related Research Articles

An active galactic nucleus (AGN) is a compact region at the center of a galaxy that emits a significant amount of energy across the electromagnetic spectrum, with characteristics indicating that this luminosity is not produced by the stars. Such excess, non-stellar emissions have been observed in the radio, microwave, infrared, optical, ultra-violet, X-ray and gamma ray wavebands. A galaxy hosting an AGN is called an active galaxy. The non-stellar radiation from an AGN is theorized to result from the accretion of matter by a supermassive black hole at the center of its host galaxy.

<span class="mw-page-title-main">Seyfert galaxy</span> Class of active galaxies with very bright nuclei

Seyfert galaxies are one of the two largest groups of active galaxies, along with quasar host galaxies. They have quasar-like nuclei with very high surface brightnesses whose spectra reveal strong, high-ionisation emission lines, but unlike quasars, their host galaxies are clearly detectable.

<span class="mw-page-title-main">Black Eye Galaxy</span> Spiral galaxy in the constellation Coma Berenices

The Black Eye Galaxy is a relatively isolated spiral galaxy 17 million light-years away in the mildly northern constellation of Coma Berenices. It was discovered by Edward Pigott in March 1779, and independently by Johann Elert Bode in April of the same year, as well as by Charles Messier the next year. A dark band of absorbing dust partially in front of its bright nucleus gave rise to its nicknames of the "Black Eye", "Evil Eye", or "Sleeping Beauty" galaxy. M64 is well known among amateur astronomers due to its form in small telescopes and visibility across inhabited latitudes.

<span class="mw-page-title-main">NGC 3227</span> Galaxy in the constellation Leo

NGC 3227 is an intermediate spiral galaxy that is interacting with the dwarf elliptical galaxy NGC 3226. The two galaxies are one of several examples of a spiral with a dwarf elliptical companion that are listed in the Atlas of Peculiar Galaxies. Both galaxies may be found in the constellation Leo. It is a member of the NGC 3227 Group of galaxies, which is a member of the Leo II Groups, a series of galaxies and galaxy clusters strung out from the right edge of the Virgo Supercluster.

<span class="mw-page-title-main">NGC 1672</span> Galaxy in the constellation Dorado

NGC 1672 is a barred spiral galaxy located in the constellation Dorado. It was discovered by the astronomer James Dunlop on November 5, 1826. It was originally unclear whether it was a member of the Dorado Group, with some sources finding it to be a member and other sources rejecting its membership. However, recent tip of the red-giant branch (TRGB) measurements indicate that NGC 1672 is located at the same distance as other members, suggesting it is indeed a member of the Dorado Group.

<span class="mw-page-title-main">NGC 4102</span> Galaxy in the constellation Ursa Major

NGC 4102 is an intermediate barred spiral galaxy located in the northern constellation of Ursa Major. It is visible in a small telescope and has an apparent visual magnitude of 11.2. The galaxy was discovered April 12, 1789 by William Herschel. J. L. E. Dreyer described it as "bright, pretty small, round, brighter middle and bright nucleus". This galaxy is located at a distance of 60 million light years and is receding with a heliocentric radial velocity of 837 km/s. It is a member of the Ursa Major group of galaxies.

<span class="mw-page-title-main">NGC 5643</span> Galaxy in the constellation Lupus

NGC 5643 is an intermediate spiral galaxy in the constellation Lupus. Based on the tip of the red-giant branch distance indicator, it is located at a distance of about 40 million light-years. NGC 5643 has an active galactic nucleus and is a type II Seyfert galaxy.

<span class="mw-page-title-main">NGC 708</span> Galaxy in the constellation Andromeda

NGC 708 is an elliptical galaxy located 240 million light-years away in the constellation Andromeda and was discovered by astronomer William Herschel on September 21, 1786. It is classified as a cD galaxy and is the brightest member of Abell 262. NGC 708 is a weak FR I radio galaxy and is also classified as a type 2 Seyfert galaxy.

<span class="mw-page-title-main">NGC 7469</span> Galaxy located in the constellation Pegasus

NGC 7469 is an intermediate spiral galaxy in the constellation of Pegasus. NGC 7469 is located about 200 million light-years away from Earth, which means, given its apparent dimensions, that NGC 7469 is approximately 90,000 light-years across. It was discovered by William Herschel on November 12, 1784.

<span class="mw-page-title-main">NGC 3367</span> Spiral galaxy in the constellation Leo

NGC 3367 is a barred spiral galaxy located in the constellation Leo. It is located at a distance of about 120 million light years from Earth, which, given its apparent dimensions, means that NGC 3367 is about 85,000 light years across. It was discovered by William Herschel on March 19, 1784.

<span class="mw-page-title-main">NGC 1380</span> Galaxy in the constellation Fornax

NGC 1380 is a lenticular galaxy located in the constellation Fornax. It is located at a distance of circa 60 million light years from Earth, which, given its apparent dimensions, means that NGC 1380 is about 85,000 light years across. It was discovered by James Dunlop on September 2, 1826. It is a member of the Fornax Cluster.

<span class="mw-page-title-main">NGC 6951</span> Galaxy in the constellation Cepheus

NGC 6951 is a barred spiral galaxy located in the constellation Cepheus. It is located at a distance of about 75 million light-years from Earth, which, given its apparent dimensions, means that NGC 6951 is about 100,000 light-years across. It was discovered by Jérôme Eugène Coggia in 1877 and independently by Lewis Swift in 1878.

<span class="mw-page-title-main">NGC 2273</span> Galaxy in the constellation Lynx

NGC 2273 is a barred spiral galaxy located in the constellation Lynx. It is located at a distance of circa 95 million light years from Earth, which, given its apparent dimensions, means that NGC 2273 is about 100,000 light years across. It was discovered by Nils Dunér on September 15, 1867.

<span class="mw-page-title-main">NGC 5728</span> Spiral galaxy in the constellation Libra

NGC 5728 is an active barred spiral galaxy located 146 million light years away in the southern constellation of Libra. It was discovered on May 7, 1787 by William Herschel. The designation comes from the New General Catalogue of J. L. E. Dreyer, published in 1888. It has an apparent visual magnitude of 13.40 and spans an angle of 3.4 arcminutes. The galaxy shows a red shift of 0.00935 and has a heliocentric radial velocity of 2,803 km/s. It has an estimated mass of 72 billion times the mass of the Sun and stretches around 30 kpc across.

<span class="mw-page-title-main">NGC 7679</span> Galaxy in the constellation Pisces

NGC 7679 is a lenticular galaxy with a peculiar morphology in the constellation Pisces. It is located at a distance of about 200 million light years from Earth, which, given its apparent dimensions, means that NGC 7679 is about 60,000 light years across. It was discovered by Heinrich d'Arrest on September 23, 1864. The total infrared luminosity is 1011.05 L☉, and thus it is categorised as a luminous infrared galaxy. NGC 7679 is both a starburst galaxy and a Seyfert galaxy.

<span class="mw-page-title-main">NGC 3516</span> Galaxy in the constellation of Ursa Major

NGC 3516 is a barred lenticular galaxy in the constellation of Ursa Major. NGC 3516 is located about 150 million light years away from Earth, which means, given its apparent dimensions, that NGC 3516 is approximately 100,000 light years across. It was discovered by William Herschel on April 3, 1785.

<span class="mw-page-title-main">NGC 4253</span> Galaxy in the constellation of Coma Berenices

NGC 4253 is a barred spiral galaxy located in the constellation Coma Berenices. It is located at a distance of about 185 million light years from Earth, which, given its apparent dimensions, means that NGC 4253 is about 65,000 light years across. It was discovered by William Herschel on February 3, 1788. It is a Seyfert galaxy.

<span class="mw-page-title-main">NGC 2110</span> Galaxy in the constellation Orion

NGC 2110 is a lenticular galaxy located in the constellation Orion. It is located at a distance of about 120 million light years from Earth, which, given its apparent dimensions, means that NGC 2110 is about 90,000 light years across. It was discovered by William Herschel on October 5, 1785. It is a Seyfert galaxy.

<span class="mw-page-title-main">NGC 3786</span> Galaxy in the constellation Ursa Major

NGC 3786 is an intermediate spiral galaxy located 107.5 million light-years away in the northern constellation of Ursa Major. It was discovered by English astronomer John Herschel on April 10, 1831. This object appears to form a close pair with its peculiar neighbor to the north, NGC 3788. They show some indications of interaction, such as minor distortion of the disk or tidal features.

<span class="mw-page-title-main">NGC 5273</span> Galaxy in the constellation Canes Venatici

NGC 5273 is a lenticular galaxy located 54 million light-years away in the northern constellation of Canes Venatici. This galaxy was discovered by William Herschel on May 1, 1785. It is positioned 1+1⁄4° to the southeast of the star 25 Canum Venaticorum.

References

  1. 1 2 3 4 5 6 7 8 "NASA/IPAC Extragalactic Database". Results for NGC 1386. Retrieved 2016-01-18.
  2. 1 2 Comerón, 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. S2CID   119295831.
  3. ↑ Seligman, Courtney. "NGC 1386 (= PGC 13333 = FCC 179)". Celestial Atlas. Retrieved 19 November 2018.
  4. ↑ Steinicke, Wolfgang (2010). Observing and Cataloguing Nebulae and Star Clusters: From Herschel to Dreyer's New General Catalogue. Cambridge University Press. pp. 258–261. ISBN   9781139490108.
  5. ↑ Sandage, A., Bedke, J. (1994), The Carnegie Atlas of Galaxies. Volume I, Carnegie Institution of Washington
  6. 1 2 Weaver, 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.
  7. 1 2 3 Ferruit, Pierre; Wilson, Andrew S.; Mulchaey, John (May 2000). "Hubble Space Telescope WFPC2 Imaging of a Sample of Early-Type Seyfert Galaxies". The Astrophysical Journal Supplement Series. 128 (1): 139–169. Bibcode:2000ApJS..128..139F. doi: 10.1086/313379 .
  8. ↑ Fuller, C.; Davies, J. I.; Auld, R.; Smith, M. W. L.; Baes, M.; Bianchi, S.; Bocchio, M.; Boselli, A.; Clemens, M.; Davis, T. A.; De Looze, I.; di Serego Alighieri, S.; Grossi, M.; Hughes, T. M.; Viaene, S.; Serra, P. (March 2014). "The Herschel Fornax Cluster Survey II: FIR properties of optically selected Fornax cluster galaxies". Monthly Notices of the Royal Astronomical Society. 440 (2): 1571–1589. arXiv: 1403.0589 . Bibcode:2014MNRAS.440.1571F. doi: 10.1093/mnras/stu369 . S2CID   53343877.
  9. 1 2 Lena, 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. S2CID   58937575.
  10. ↑ Woo, Jong-Hak; Urry, C. Megan (10 November 2002). "Active Galactic Nucleus Black Hole Masses and Bolometric Luminosities". The Astrophysical Journal. 579 (2): 530–544. arXiv: astro-ph/0207249 . Bibcode:2002ApJ...579..530W. doi:10.1086/342878. S2CID   118160249.
  11. ↑ Mundell, C. G.; Ferruit, P.; Nagar, N.; Wilson, A. S. (20 September 2009). "Radio Variability in Seyfert Nuclei". The Astrophysical Journal. 703 (1): 802–815. arXiv: 0907.1489 . Bibcode:2009ApJ...703..802M. doi:10.1088/0004-637X/703/1/802. S2CID   2430781.
  12. ↑ Ruschel-Dutra, Daniel; Pastoriza, Miriani; Riffel, Rogério; Sales, Dinalva A.; Winge, Cláudia (11 March 2014). "A mid-IR comparative analysis of the Seyfert galaxies NGC 7213 and NGC 1386". Monthly Notices of the Royal Astronomical Society. 438 (4): 3434–3442. arXiv: 1401.1989 . Bibcode:2014MNRAS.438.3434R. doi: 10.1093/mnras/stt2448 . S2CID   73527369.
  13. ↑ 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. ISSN   0004-6361.
  14. 1 2 Levenson, N. A.; Heckman, T. M.; Krolik, J. H.; Weaver, K. A.; Życki, P. T. (September 2006). "Penetrating the Deep Cover of Compton-thick Active Galactic Nuclei". The Astrophysical Journal. 648 (1): 111–127. arXiv: astro-ph/0605438 . Bibcode:2006ApJ...648..111L. doi:10.1086/505735. S2CID   16434679.
  15. ↑ 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. S2CID   43332114.
  16. ↑ 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. S2CID   7842878.
  17. ↑ Li, Jiang-Tao; Wang, Q. Daniel (21 January 2013). "Chandra survey of nearby highly inclined disc galaxies – I. X-ray measurements of galactic coronae". Monthly Notices of the Royal Astronomical Society. 428 (3): 2085–2108. arXiv: 1210.2997 . Bibcode:2013MNRAS.428.2085L. doi: 10.1093/mnras/sts183 . S2CID   119109532.
  18. ↑ 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.
  19. ↑ 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 . S2CID   123352311.
  20. ↑ Bennert, N.; Jungwiert, B.; Komossa, S.; Haas, M.; Chini, R. (20 January 2006). "Size and properties of the NLR in the Seyfert-2 galaxy NGC 1386". Astronomy & Astrophysics. 446 (3): 919–932. arXiv: astro-ph/0511279 . doi: 10.1051/0004-6361:20053571 .
  21. ↑ 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. S2CID   118855983.
  22. ↑ 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.
  23. ↑ Makarov, Dmitry; Karachentsev, Igor (21 April 2011). "Galaxy groups and clouds in the local (z~ 0.01) Universe". Monthly Notices of the Royal Astronomical Society. 412 (4): 2498–2520. arXiv: 1011.6277 . Bibcode:2011MNRAS.412.2498M. doi: 10.1111/j.1365-2966.2010.18071.x . S2CID   119194025.
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