NGC 1386

{{Infobox galaxy

| name = NGC 1386

| image = NGC 1386 -HST06419 02R791GB658n.png

| upright = 1.15

| caption = NGC 1386 by the Hubble Space Telescope

| credit = ESA/NASA

| epoch = J2000

| type = ({{prime|R}})SA(r)0/a

| ra = {{RA|03|36|46.2}}

| dec = {{DEC|-35|59|58}}

| dist_ly = 52.6 ± 2.3 Mly (16.2 ± 0.7 Mpc){{cite web

| title=NASA/IPAC Extragalactic Database

| work=Results for NGC 1386

| url=http://ned.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=NGC+1386

| access-date=2016-01-18 }}

| z = 0.002895 ± 0.000017

| h_radial_v = 868 ± 5 km/s

| appmag_v = 11.2

| size_v = 3.4{{prime}} × 1.3{{prime}}

| group_cluster = Fornax cluster

| constellation name = Eridanus

| notes = Seyfert galaxy

| names = ESO 358- G035, FCC 179, MCG -06-09-005, PGC 13333

}}

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. It is a Seyfert galaxy, the only one in Fornax Cluster.

Observation history

NGC 1386 was discovered by Johann Friedrich Julius Schmidt on January 19, 1865.{{cite web |last1=Seligman |first1=Courtney |title=NGC 1386 (= PGC 13333 = FCC 179) |url=https://cseligman.com/text/atlas/ngc13a.htm#1386 |website=Celestial Atlas |access-date=19 November 2018}} 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.{{cite book |last1=Steinicke |first1=Wolfgang |title=Observing and Cataloguing Nebulae and Star Clusters: From Herschel to Dreyer's New General Catalogue |date=2010 |publisher=Cambridge University Press |isbn=9781139490108 |pages=258–261 |url=https://books.google.com/books?id=wyWjVWYWoO8C&pg=PA260 |language=en}}

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,Sandage, A., Bedke, J. (1994), The Carnegie Atlas of Galaxies. Volume I, Carnegie Institution of Washington however HII emission has been detected in the arms.{{cite journal |last1=Weaver |first1=K. A. |last2=Wilson |first2=A. S. |last3=Baldwin |first3=J. A. |title=Kinematics and ionization of extended gas in active galaxies. VI - The Seyfert 2 galaxy NGC 1386 |journal=The Astrophysical Journal |date=January 1991 |volume=366 |pages=50 |doi=10.1086/169539|bibcode=1991ApJ...366...50W }} Dust features have also being observed at the central region of the galaxy.{{cite journal |last1=Ferruit |first1=Pierre |last2=Wilson |first2=Andrew S. |last3=Mulchaey |first3=John |title=Hubble Space Telescope WFPC2 Imaging of a Sample of Early-Type Seyfert Galaxies |journal=The Astrophysical Journal Supplement Series |date=May 2000 |volume=128 |issue=1 |pages=139–169 |doi=10.1086/313379|bibcode=2000ApJS..128..139F |doi-access=free }} Based on observations by the Herschel Space Telescope the total dust mass of NGC 1386 is estimated to be {{val|e=6.78|ul=M_solar}} and the stellar mass {{val|e=10.5|ul=M_solar}}.{{cite journal |last1=Fuller |first1=C. |last2=Davies |first2=J. I. |last3=Auld |first3=R. |last4=Smith |first4=M. W. L. |last5=Baes |first5=M. |last6=Bianchi |first6=S. |last7=Bocchio |first7=M. |last8=Boselli |first8=A. |last9=Clemens |first9=M. |last10=Davis |first10=T. A. |last11=De Looze |first11=I. |last12=di Serego Alighieri |first12=S. |last13=Grossi |first13=M. |last14=Hughes |first14=T. M. |last15=Viaene |first15=S. |last16=Serra |first16=P. |title=The Herschel Fornax Cluster Survey II: FIR properties of optically selected Fornax cluster galaxies |journal=Monthly Notices of the Royal Astronomical Society |date=March 2014 |volume=440 |issue=2 |pages=1571–1589 |doi=10.1093/mnras/stu369|doi-access=free |bibcode=2014MNRAS.440.1571F |arxiv=1403.0589 |s2cid=53343877 }} The galaxy has two ring structures, with diameters of 0.5 and 1.67 arcminutes.{{cite journal |last1=Comerón |first1=S. |last2=Salo |first2=H. |last3=Laurikainen |first3=E. |last4=Knapen |first4=J. H. |last5=Buta |first5=R. J. |last6=Herrera-Endoqui |first6=M. |last7=Laine |first7=J. |last8=Holwerda |first8=B. W. |last9=Sheth |first9=K. |last10=Regan |first10=M. W. |last11=Hinz |first11=J. L. |last12=Muñoz-Mateos |first12=J. C. |last13=Gil de Paz |first13=A. |last14=Menéndez-Delmestre |first14=K. |last15=Seibert |first15=M. |last16=Mizusawa |first16=T. |last17=Kim |first17=T. |last18=Erroz-Ferrer |first18=S. |last19=Gadotti |first19=D. A. |last20=Athanassoula |first20=E. |author20-link=Lia Athanassoula|last21=Bosma |first21=A. |last22=Ho |first22=L. C. |title=ARRAKIS: atlas of resonance rings as known in the S4G |journal=Astronomy & Astrophysics |date=19 February 2014 |volume=562 |pages=A121 |doi=10.1051/0004-6361/201321633|arxiv=1312.0866 |bibcode=2014A&A...562A.121C |s2cid=119295831 }}

= Active galactic nucleus =

NGC 1386 has an active galactic nucleus (AGN) that has been categorised as a type 2 Seyfert galaxy. 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.{{cite journal |last1=Lena |first1=D. |last2=Robinson |first2=A. |last3=Storchi-Bergman |first3=T. |last4=Schnorr-Müller |first4=A. |last5=Seelig |first5=T. |last6=Riffel |first6=R. A. |last7=Nagar |first7=N. M. |last8=Couto |first8=G. S. |last9=Shadler |first9=L. |title=The Complex Gas Kinematics in the Nucleus of the Seyfert 2 Galaxy NGC 1386: Rotation, Outflows, and Inflows |journal=The Astrophysical Journal |date=9 June 2015 |volume=806 |issue=1 |pages=84 |doi=10.1088/0004-637X/806/1/84|bibcode=2015ApJ...806...84L |arxiv=1504.05089 |s2cid=58937575 }} The black hole in the centre of NGC 1386 is estimated to be {{val|2.6|e=7|ul=M_solar}} based on stellar velocity dispersion.{{cite journal |last1=Woo |first1=Jong-Hak |last2=Urry |first2=C. Megan |title=Active Galactic Nucleus Black Hole Masses and Bolometric Luminosities |journal=The Astrophysical Journal |date=10 November 2002 |volume=579 |issue=2 |pages=530–544 |doi=10.1086/342878|bibcode=2002ApJ...579..530W |arxiv=astro-ph/0207249 |s2cid=118160249 }}

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 {{solar mass}} 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.

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.{{cite journal |last1=Mundell |first1=C. G. |title=Radio Variability in Seyfert Nuclei |last2=Ferruit |first2=P. |last3=Nagar |first3=N. |last4=Wilson |first4=A. S. |journal=The Astrophysical Journal |date=20 September 2009 |volume=703 |issue=1 |pages=802–815 |doi=10.1088/0004-637X/703/1/802|bibcode=2009ApJ...703..802M |arxiv=0907.1489 |s2cid=2430781 }} 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. 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.{{cite journal |last1=Ruschel-Dutra |first1=Daniel |last2=Pastoriza |first2=Miriani |last3=Riffel |first3=Rogério |last4=Sales |first4=Dinalva A. |last5=Winge |first5=Cláudia |title=A mid-IR comparative analysis of the Seyfert galaxies NGC 7213 and NGC 1386 |journal=Monthly Notices of the Royal Astronomical Society |date=11 March 2014 |volume=438 |issue=4 |pages=3434–3442 |doi=10.1093/mnras/stt2448|doi-access=free |bibcode=2014MNRAS.438.3434R |arxiv=1401.1989 |s2cid=73527369 }}

File:VST image of the Fornax Galaxy Cluster.jpg. 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,{{cite journal |last1=Maiolino |first1=R. |last2=Salvati |first2=M. |last3=Bassani |first3=L. |last4=Dadina |first4=M. |last5=della Ceca |first5=R. |last6=Matt |first6=G. |last7=Risaliti |first7=G. |last8=Zamorani |first8=G. |title=Heavy obscuration in X-ray weak AGNs |journal=Astronomy and Astrophysics |date=1 October 1998 |volume=338 |pages=781–794 |issn=0004-6361 |bibcode=1998A&A...338..781M|arxiv=astro-ph/9806055 }}{{cite journal |last1=Levenson |first1=N. A. |last2=Heckman |first2=T. M. |last3=Krolik |first3=J. H. |last4=Weaver |first4=K. A. |last5=Życki |first5=P. T. |title=Penetrating the Deep Cover of Compton-thick Active Galactic Nuclei |journal=The Astrophysical Journal |date=September 2006 |volume=648 |issue=1 |pages=111–127 |doi=10.1086/505735|bibcode=2006ApJ...648..111L |arxiv=astro-ph/0605438 |s2cid=16434679 }} estimated to be {{val|5|1|e=24}} cm⁻² as measured by NuSTAR.{{cite journal |last1=Masini |first1=A. |last2=Comastri |first2=A. |last3=Baloković |first3=M. |last4=Zaw |first4=I. |last5=Puccetti |first5=S. |last6=Ballantyne |first6=D. R. |last7=Bauer |first7=F. E. |last8=Boggs |first8=S. E. |last9=Brandt |first9=W. N. |last10=Brightman |first10=M. |last11=Christensen |first11=F. E. |last12=Craig |first12=W. W. |last13=Gandhi |first13=P. |last14=Hailey |first14=C. J. |last15=Harrison |first15=F. A. |last16=Koss |first16=M. J. |last17=Madejski |first17=G. |last18=Ricci |first18=C. |last19=Rivers |first19=E. |last20=Stern |first20=D. |last21=Zhang |first21=W. W. |title=NuSTAR observations of water megamaser AGN |journal=Astronomy & Astrophysics |date=13 April 2016 |volume=589 |pages=A59 |doi=10.1051/0004-6361/201527689|bibcode=2016A&A...589A..59M |arxiv=1602.03185 |s2cid=43332114 }} The observations imply that the torus covers much of the nucleus.{{cite journal |last1=Brightman |first1=M. |last2=Baloković |first2=M. |last3=Stern |first3=D. |last4=Arévalo |first4=P. |last5=Ballantyne |first5=D. R. |last6=Bauer |first6=F. E. |last7=Boggs |first7=S. E. |last8=Craig |first8=W. W. |last9=Christensen |first9=F. E. |last10=Comastri |first10=A. |last11=Fuerst |first11=F. |last12=Gandhi |first12=P. |last13=Hailey |first13=C. J. |last14=Harrison |first14=F. A. |last15=Hickox |first15=R. C. |last16=Koss |first16=M. |last17=LaMassa |first17=S. |last18=Puccetti |first18=S. |last19=Rivers |first19=E. |last20=Vasudevan |first20=R. |last21=Walton |first21=D. J. |last22=Zhang |first22=W. W. |title=Determining the Covering Factor of Compton-thick Active Galactic Nuclei with NuSTAR |journal=The Astrophysical Journal |date=19 May 2015 |volume=805 |issue=1 |pages=41 |doi=10.1088/0004-637X/805/1/41|bibcode=2015ApJ...805...41B |arxiv=1502.07353 |s2cid=7842878 }} 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. NGC 1386 has a corona with faint diffuse soft X-ray emission that appears distorted at its outer parts.{{cite journal |last1=Li |first1=Jiang-Tao |last2=Wang |first2=Q. Daniel |title=Chandra survey of nearby highly inclined disc galaxies – I. X-ray measurements of galactic coronae |journal=Monthly Notices of the Royal Astronomical Society |date=21 January 2013 |volume=428 |issue=3 |pages=2085–2108 |doi=10.1093/mnras/sts183|doi-access=free |bibcode=2013MNRAS.428.2085L |arxiv=1210.2997 |s2cid=119109532 }}

NGC 1386 has been found to host a cosmic water maser.{{cite journal |last1=Braatz |first1=J. |last2=Greenhill |first2=L. |last3=Moran |first3=J. |last4=Wilson |first4=A. |last5=Herrnstein |first5=J. |title=A VLBA Map of the H_2O Maser in the Nucleus of Seyfert 2 Galaxy NGC 1386 |journal=American Astronomical Society Meeting Abstracts |date=1 December 1997 |volume=191 |pages=104.02 |bibcode=1997AAS...19110402B}} It also features a HII region at the circumnuclear region.{{cite journal |last1=Storchi-Bergmann |first1=Thaisa |last2=Rodriguez-Ardila |first2=Alberto |last3=Schmitt |first3=Henrique R. |last4=Wilson |first4=Andrew S. |last5=Baldwin |first5=Jack A. |title=Circumnuclear Star Formation in Active Galaxies |journal=The Astrophysical Journal |date=20 November 1996 |volume=472 |issue=1 |pages=83–101 |doi=10.1086/178043|bibcode=1996ApJ...472...83S |hdl=10183/108769 |s2cid=123352311 |hdl-access=free }} 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.{{cite journal |last1=Bennert |first1=N. |last2=Jungwiert |first2=B. |last3=Komossa |first3=S. |last4=Haas |first4=M. |last5=Chini |first5=R. |title=Size and properties of the NLR in the Seyfert-2 galaxy NGC 1386 |journal=Astronomy & Astrophysics |date=20 January 2006 |volume=446 |issue=3 |pages=919–932 |doi=10.1051/0004-6361:20053571 | arxiv=astro-ph/0511279 |doi-access=free }} 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.

Nearby galaxies

NGC 1386 is considered to be part of the Fornax Cluster.{{cite journal |last1=Sarzi |first1=M. |last2=Iodice |first2=E. |last3=Coccato |first3=L. |last4=Corsini |first4=E. M. |last5=de Zeeuw |first5=P. T. |last6=Falcón-Barroso |first6=J. |last7=Gadotti |first7=D. A. |last8=Lyubenova |first8=M. |last9=McDermid |first9=R. M. |last10=de Ven |first10=G. van |last11=Fahrion |first11=K. |last12=Pizzella |first12=A. |last13=Zhu |first13=L. |title=Fornax3D project: Overall goals, galaxy sample, MUSE data analysis, and initial results |journal=Astronomy & Astrophysics |date=28 August 2018 |volume=616 |pages=A121 |doi=10.1051/0004-6361/201833137|arxiv=1804.06795|bibcode=2018A&A...616A.121S |s2cid=118855983 }} 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.{{cite journal |last1=Rossa |first1=J. |last2=Dietrich |first2=M. |last3=Wagner |first3=S.J. |title=Kinematics and morphology of the Narrow-Line Region in the Seyfert galaxy NGC1386 |journal=Astronomy and Astrophysics |date=October 2000 |volume=362 |pages=501–508 |bibcode=2000A&A...362..501R|arxiv=astro-ph/0008269}} Makarov and Karachentsev grouped NGC 1386 in the NGC 1386 group, along with NGC 1389 and NGC 1396.{{cite journal|last1=Makarov|first1=Dmitry|last2=Karachentsev|first2=Igor|title=Galaxy groups and clouds in the local (z~ 0.01) Universe|journal=Monthly Notices of the Royal Astronomical Society|date=21 April 2011|volume=412|issue=4|pages=2498–2520|doi=10.1111/j.1365-2966.2010.18071.x|doi-access=free |bibcode=2011MNRAS.412.2498M|arxiv=1011.6277|s2cid=119194025}}