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{{Short description|Elliptical galaxy in the constellation Eridanus}}
{{Short description|Galaxy in the constellation Eridanus}}
{{Infobox galaxy
{{Infobox galaxy
| name = [[New General Catalogue|NGC]] 1395
| name = [[New General Catalogue|NGC]] 1395
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| h_radial_v = 1,717 ± 7 [[kilometer|km]]/[[second|s]]<ref name="ned" />
| h_radial_v = 1,717 ± 7 [[kilometer|km]]/[[second|s]]<ref name="ned" />
| appmag_v = 9.8
| appmag_v = 9.8
| size_v = 5&prime;.9 × 4&prime;.5<ref name="ned" />
| size_v = 5.9{{prime}} × 4.5{{prime}}<ref name="ned" />
| constellation name = [[Eridanus (constellation)|Eridanus]]
| constellation name = [[Eridanus (constellation)|Eridanus]]
| notes =
| notes =
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== Characteristics ==
== Characteristics ==
In the centre of NGC 1395 lies a [[supermassive black hole]] whose mass is estimated to be {{val|3.9|e=8}} (10<sup>8.59</sup>) {{solar mass|link=yes}} based on the [[M–sigma relation]]<ref>{{cite journal |last1=Pellegrini |first1=S. |title=The Nuclear X-ray Emission of Nearby Early-type Galaxies |journal=The Astrophysical Journal |date=2010 |volume=717 |issue=2 |pages=640–652 |doi=10.1088/0004-637X/717/2/640 |language=en |issn=0004-637X|bibcode=2010ApJ...717..640P |arxiv=1005.2344 |s2cid=119289831 }}</ref> or between 100 and 257 million (10<sup>8</sup> – 10<sup>8.41</sup>) {{solar mass}} based on the [[Sersic profile|Sérsic index]] of the galaxy.<ref>{{cite journal |last1=Mutlu-Pakdil |first1=Burçin |last2=Seigar |first2=Marc S. |last3=Davis |first3=Benjamin L. |title=The local black hole mass function derived from the MBH-P and the MBH-n relations |journal=The Astrophysical Journal |date=17 October 2016 |volume=830 |issue=2 |pages=117 |doi=10.3847/0004-637X/830/2/117|bibcode=2016ApJ...830..117M |arxiv=1607.07325 |s2cid=118586684 }}</ref> NGC 1395 emits [[X-ray]]s which have been observed by [[Chandra X-ray Observatory]] and [[XMM-Newton]]. The luminosity of the galaxy in X-rays is {{val|3|e=40}} ergs and is believed it is emitted by hot gas with total mass {{val|4.1|e=8|u=M_solar}}.<ref>{{cite journal |last1=Su |first1=Yuanyuan |last2=Irwin |first2=Jimmy A. |title=Investigating the potential dilution of the metal content of hot gas in early-type galaxies by accreted cold gas |journal=The Astrophysical Journal |date=7 March 2013 |volume=766 |issue=1 |pages=61 |doi=10.1088/0004-637X/766/1/61|bibcode=2013ApJ...766...61S |arxiv=1301.7706 |s2cid=118617980 }}</ref> One other source of X-ray emission in [[Hubble sequence|early type galaxies]] are [[X-ray binaries|X-ray binary stars]], with 24 sources being detected in the inner area of NGC 1395.<ref>{{cite journal |last1=Vagshette |first1=N.D. |last2=Pandge |first2=M.B. |last3=Patil |first3=M.K. |title=Spectral properties of XRBs in dusty early-type galaxies |journal=New Astronomy |date=July 2013 |volume=21 |pages=1–7 |doi=10.1016/j.newast.2012.10.005|arxiv=1205.6057|bibcode=2013NewA...21....1V |s2cid=119198114 }}</ref>
In the centre of NGC 1395 lies a [[supermassive black hole]] whose mass is estimated to be {{val|3.9|e=8}} (10<sup>8.59</sup>) {{solar mass|link=yes}} based on the [[M–sigma relation]]<ref>{{cite journal |last1=Pellegrini |first1=S. |title=The Nuclear X-ray Emission of Nearby Early-type Galaxies |journal=The Astrophysical Journal |date=2010 |volume=717 |issue=2 |pages=640–652 |doi=10.1088/0004-637X/717/2/640 |language=en |issn=0004-637X|bibcode=2010ApJ...717..640P |arxiv=1005.2344 |s2cid=119289831 }}</ref> or between 100 and 257 million (10<sup>8</sup> – 10<sup>8.41</sup>) {{solar mass}} based on the [[Sersic profile|Sérsic index]] of the galaxy.<ref>{{cite journal |last1=Mutlu-Pakdil |first1=Burçin |last2=Seigar |first2=Marc S. |last3=Davis |first3=Benjamin L. |title=The local black hole mass function derived from the MBH-P and the MBH-n relations |journal=The Astrophysical Journal |date=17 October 2016 |volume=830 |issue=2 |pages=117 |doi=10.3847/0004-637X/830/2/117|bibcode=2016ApJ...830..117M |arxiv=1607.07325 |s2cid=118586684 |doi-access=free }}</ref> NGC 1395 emits [[X-ray]]s which have been observed by [[Chandra X-ray Observatory]] and [[XMM-Newton]]. The luminosity of the galaxy in X-rays is {{val|3|e=40}} ergs and is believed it is emitted by hot gas with total mass {{val|4.1|e=8|u=M_solar}}.<ref>{{cite journal |last1=Su |first1=Yuanyuan |last2=Irwin |first2=Jimmy A. |title=Investigating the potential dilution of the metal content of hot gas in early-type galaxies by accreted cold gas |journal=The Astrophysical Journal |date=7 March 2013 |volume=766 |issue=1 |pages=61 |doi=10.1088/0004-637X/766/1/61|bibcode=2013ApJ...766...61S |arxiv=1301.7706 |s2cid=118617980 }}</ref> One other source of X-ray emission in [[Hubble sequence|early type galaxies]] are [[X-ray binaries|X-ray binary stars]], with 24 sources being detected in the inner area of NGC 1395.<ref>{{cite journal |last1=Vagshette |first1=N.D. |last2=Pandge |first2=M.B. |last3=Patil |first3=M.K. |title=Spectral properties of XRBs in dusty early-type galaxies |journal=New Astronomy |date=July 2013 |volume=21 |pages=1–7 |doi=10.1016/j.newast.2012.10.005|arxiv=1205.6057|bibcode=2013NewA...21....1V |s2cid=119198114 }}</ref>


NGC 1395 is home to a large number of [[globular cluster]]s, with their total number estimated to be {{val|6000|1100}}, compared to 150–200 in and around the [[Milky Way]]. There are two different populations of globular clusters in the galaxy, named blue and red from their photometric color. The clusters of the red subpopulation lie closer to the centre of the galaxy while the blue ones lie mostly in the halo. The surface density profile of the blue globular clusters indicates that the galaxy has accreted a significant number of dwarf satellites.<ref name="Escudero2018">{{cite journal |last1=Escudero |first1=Carlos G |last2=Faifer |first2=Favio R |last3=Smith Castelli |first3=Analía V |last4=Forte |first4=Juan C |last5=Sesto |first5=Leandro A |last6=González |first6=Nélida M |last7=Scalia |first7=María C |title=Tracing the assembly history of NGC 1395 through its Globular Cluster System |journal=Monthly Notices of the Royal Astronomical Society |date=March 2018 |volume=474 |issue=4 |pages=4302–4321 |doi=10.1093/mnras/stx3045|bibcode=2018MNRAS.474.4302E |arxiv=1711.08046 }}</ref>
NGC 1395 is home to a large number of [[globular cluster]]s, with their total number estimated to be {{val|6000|1100}}, compared to 150–200 in and around the [[Milky Way]]. There are two different populations of globular clusters in the galaxy, named blue and red from their photometric color. The clusters of the red subpopulation lie closer to the centre of the galaxy while the blue ones lie mostly in the halo. The surface density profile of the blue globular clusters indicates that the galaxy has accreted a significant number of dwarf satellites.<ref name="Escudero2018">{{cite journal |last1=Escudero |first1=Carlos G |last2=Faifer |first2=Favio R |last3=Smith Castelli |first3=Analía V |last4=Forte |first4=Juan C |last5=Sesto |first5=Leandro A |last6=González |first6=Nélida M |last7=Scalia |first7=María C |title=Tracing the assembly history of NGC 1395 through its Globular Cluster System |journal=Monthly Notices of the Royal Astronomical Society |date=March 2018 |volume=474 |issue=4 |pages=4302–4321 |doi=10.1093/mnras/stx3045|doi-access=free |bibcode=2018MNRAS.474.4302E |arxiv=1711.08046 }}</ref>


[[David Malin]] and Dave Carter discovered in 1983 low contrast [[shell galaxy|shells]] in the bright envelope of NGC 1395.<ref>{{cite journal |last1=Malin |first1=D. F. |last2=Carter |first2=D. |title=A catalog of elliptical galaxies with shells |journal=The Astrophysical Journal |date=November 1983 |volume=274 |pages=534 |doi=10.1086/161467|bibcode=1983ApJ...274..534M }}</ref> The brightest shell lies 3 arcminutes northwest of the galactic centre.<ref name="Escudero2018"/> A perpendicular feature is seen also in deep imaging in the northwest part of the galaxy.<ref>{{cite journal |last1=Tal |first1=Tomer |last2=van Dokkum |first2=Pieter G. |last3=Nelan |first3=Jenica |last4=Bezanson |first4=Rachel |title=The Frequency of Tidal Features Associated with Nearby Luminous Elliptical Galaxies from a Statistically Complete Sample |journal=The Astronomical Journal |date=1 November 2009 |volume=138 |issue=5 |pages=1417–1427 |doi=10.1088/0004-6256/138/5/1417|bibcode=2009AJ....138.1417T |arxiv=0908.1382 |s2cid=19104100 }}</ref> Features like these are indicative of recent [[galaxy merger|accretion]] of a smaller galaxy in the recent past.<ref name="Escudero2018"/>
[[David Malin]] and Dave Carter discovered in 1983 low contrast [[shell galaxy|shells]] in the bright envelope of NGC 1395.<ref>{{cite journal |last1=Malin |first1=D. F. |last2=Carter |first2=D. |title=A catalog of elliptical galaxies with shells |journal=The Astrophysical Journal |date=November 1983 |volume=274 |pages=534 |doi=10.1086/161467|bibcode=1983ApJ...274..534M |doi-access=free }}</ref> The brightest shell lies 3 arcminutes northwest of the galactic centre.<ref name="Escudero2018"/> A perpendicular feature is seen also in deep imaging in the northwest part of the galaxy.<ref>{{cite journal |last1=Tal |first1=Tomer |last2=van Dokkum |first2=Pieter G. |last3=Nelan |first3=Jenica |last4=Bezanson |first4=Rachel |title=The Frequency of Tidal Features Associated with Nearby Luminous Elliptical Galaxies from a Statistically Complete Sample |journal=The Astronomical Journal |date=1 November 2009 |volume=138 |issue=5 |pages=1417–1427 |doi=10.1088/0004-6256/138/5/1417|bibcode=2009AJ....138.1417T |arxiv=0908.1382 |s2cid=19104100 }}</ref> Features like these are indicative of recent [[galaxy merger|accretion]] of a smaller galaxy in the recent past.<ref name="Escudero2018"/>


== Nearby galaxies ==
== Nearby galaxies ==
NGC 1395 is part of the [[Eridanus Cluster]] and is the brightest member of the NGC 1395 subgroup. Other members of this subgroup are the galaxies [[IC 1952]], [[NGC 1401]], [[NGC 1414]], [[NGC 1415]], [[NGC 1422]], [[NGC 1426]], [[NGC 1438]], and [[NGC 1439]].<ref name=Makarov>{{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|url=http://www.sao.ru/hq/dim/groups/galaxies.dat|bibcode=2011MNRAS.412.2498M|arxiv = 1011.6277 |s2cid=119194025 }}</ref>
NGC 1395 is part of the [[Eridanus Cluster]] and is the brightest member of the NGC 1395 subgroup. Other members of this subgroup are the galaxies [[IC 1952]], [[NGC 1401]], [[NGC 1414]], [[NGC 1415]], [[NGC 1422]], [[NGC 1426]], [[NGC 1438]], and [[NGC 1439]].<ref name=Makarov>{{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}}</ref>


== References ==
== References ==

Latest revision as of 13:57, 6 September 2024

NGC 1395
NGC 1395 by PanSTARRS
Observation data (J2000 epoch)
ConstellationEridanus
Right ascension03h 38m 29.8s[1]
Declination−23° 01′ 39″[1]
Redshift0.005727 +/- 0.000022 [1]
Heliocentric radial velocity1,717 ± 7 km/s[1]
Distance74.4 ± 17.8 Mly (22.8 ± 5.4 Mpc)[1]
Apparent magnitude (V)9.8
Characteristics
TypeE2 [1]
Apparent size (V)5.9′ × 4.5′[1]
Other designations
ESO 482- G019, AM 0336-231, MCG -04-09-039, PGC 13419[1]

NGC 1395 is an elliptical galaxy located in the constellation Eridanus. It is located at a distance of circa 75 million light years from Earth, which, given its apparent dimensions, means that NGC 1395 is about 130,000 light years across.[1] It was discovered by William Herschel on November 17, 1784.[2] It is a member of the Eridanus Cluster.

Characteristics

[edit]

In the centre of NGC 1395 lies a supermassive black hole whose mass is estimated to be 3.9×108 (108.59) M☉ based on the M–sigma relation[3] or between 100 and 257 million (108 – 108.41) M☉ based on the Sérsic index of the galaxy.[4] NGC 1395 emits X-rays which have been observed by Chandra X-ray Observatory and XMM-Newton. The luminosity of the galaxy in X-rays is 3×1040 ergs and is believed it is emitted by hot gas with total mass 4.1×108 M☉.[5] One other source of X-ray emission in early type galaxies are X-ray binary stars, with 24 sources being detected in the inner area of NGC 1395.[6]

NGC 1395 is home to a large number of globular clusters, with their total number estimated to be 6000±1100, compared to 150–200 in and around the Milky Way. There are two different populations of globular clusters in the galaxy, named blue and red from their photometric color. The clusters of the red subpopulation lie closer to the centre of the galaxy while the blue ones lie mostly in the halo. The surface density profile of the blue globular clusters indicates that the galaxy has accreted a significant number of dwarf satellites.[7]

David Malin and Dave Carter discovered in 1983 low contrast shells in the bright envelope of NGC 1395.[8] The brightest shell lies 3 arcminutes northwest of the galactic centre.[7] A perpendicular feature is seen also in deep imaging in the northwest part of the galaxy.[9] Features like these are indicative of recent accretion of a smaller galaxy in the recent past.[7]

Nearby galaxies

[edit]

NGC 1395 is part of the Eridanus Cluster and is the brightest member of the NGC 1395 subgroup. Other members of this subgroup are the galaxies IC 1952, NGC 1401, NGC 1414, NGC 1415, NGC 1422, NGC 1426, NGC 1438, and NGC 1439.[10]

References

[edit]
  1. ^ a b c d e f g h i "NASA/IPAC Extragalactic Database". Results for NGC 1395. Retrieved 2016-01-18.
  2. ^ Seligman, Courtney. "NGC 1395 (= PGC 13419)". Celestial Atlas. Retrieved 19 November 2018.
  3. ^ Pellegrini, S. (2010). "The Nuclear X-ray Emission of Nearby Early-type Galaxies". The Astrophysical Journal. 717 (2): 640–652. arXiv:1005.2344. Bibcode:2010ApJ...717..640P. doi:10.1088/0004-637X/717/2/640. ISSN 0004-637X. S2CID 119289831.
  4. ^ Mutlu-Pakdil, Burçin; Seigar, Marc S.; Davis, Benjamin L. (17 October 2016). "The local black hole mass function derived from the MBH-P and the MBH-n relations". The Astrophysical Journal. 830 (2): 117. arXiv:1607.07325. Bibcode:2016ApJ...830..117M. doi:10.3847/0004-637X/830/2/117. S2CID 118586684.
  5. ^ Su, Yuanyuan; Irwin, Jimmy A. (7 March 2013). "Investigating the potential dilution of the metal content of hot gas in early-type galaxies by accreted cold gas". The Astrophysical Journal. 766 (1): 61. arXiv:1301.7706. Bibcode:2013ApJ...766...61S. doi:10.1088/0004-637X/766/1/61. S2CID 118617980.
  6. ^ Vagshette, N.D.; Pandge, M.B.; Patil, M.K. (July 2013). "Spectral properties of XRBs in dusty early-type galaxies". New Astronomy. 21: 1–7. arXiv:1205.6057. Bibcode:2013NewA...21....1V. doi:10.1016/j.newast.2012.10.005. S2CID 119198114.
  7. ^ a b c Escudero, Carlos G; Faifer, Favio R; Smith Castelli, Analía V; Forte, Juan C; Sesto, Leandro A; González, Nélida M; Scalia, María C (March 2018). "Tracing the assembly history of NGC 1395 through its Globular Cluster System". Monthly Notices of the Royal Astronomical Society. 474 (4): 4302–4321. arXiv:1711.08046. Bibcode:2018MNRAS.474.4302E. doi:10.1093/mnras/stx3045.
  8. ^ Malin, D. F.; Carter, D. (November 1983). "A catalog of elliptical galaxies with shells". The Astrophysical Journal. 274: 534. Bibcode:1983ApJ...274..534M. doi:10.1086/161467.
  9. ^ Tal, Tomer; van Dokkum, Pieter G.; Nelan, Jenica; Bezanson, Rachel (1 November 2009). "The Frequency of Tidal Features Associated with Nearby Luminous Elliptical Galaxies from a Statistically Complete Sample". The Astronomical Journal. 138 (5): 1417–1427. arXiv:0908.1382. Bibcode:2009AJ....138.1417T. doi:10.1088/0004-6256/138/5/1417. S2CID 19104100.
  10. ^ 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.
[edit]
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