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Coordinates: Sky map 04h 45m 42.500s, −59° 14′ 49.85″
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{{short description|Barred spiral galaxy in the constellation Dorado}}
{{short description|Galaxy in the constellation Dorado}}
{{Infobox Galaxy
{{Infobox Galaxy
| name = [[New General Catalogue|NGC]] 1672
| name = [[New General Catalogue|NGC]] 1672
| image = NGC1672 - Iotw2205a.jpg
| image = NGC1672 - Iotw2205a.jpg
| image_size = 300px
| image_size = 300px
|caption = The galaxy photographed with the [[Victor M. Blanco Telescope]]
|caption = The galaxy photographed with the [[Víctor M. Blanco Telescope]]
|credit=
|credit=
| epoch = [[J2000]]
| epoch = [[J2000]]
Line 13: Line 13:
| z = 1331 ± 3 km/[[second|s]]<ref name="ned" />
| z = 1331 ± 3 km/[[second|s]]<ref name="ned" />
| appmag_v = 10.3<ref name="ned" />
| appmag_v = 10.3<ref name="ned" />
| size_v = 6&prime;.6 × 5&prime;.5<ref name="ned" />
| size_v = 6.6{{prime}} × 5.5{{prime}}<ref name="ned" />
| constellation name = [[Dorado]]
| constellation name = [[Dorado]]
| notes =
| notes =
Line 38: Line 38:
| title = A catalog of southern groups of galaxies
| title = A catalog of southern groups of galaxies
| author = Maia, M. A. G. | author2 = da Costa, L. N. | author3 = Latham, David W.
| author = Maia, M. A. G. | author2 = da Costa, L. N. | author3 = Latham, David W.
| doi-access = free
}}</ref> 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.<ref name=Tikhonov/>
}}</ref> 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.<ref name=Tikhonov/>


NGC 1672 has a large bar which is estimated to measure around 20 kpc.<ref name="Becketal2002">{{Cite journal
NGC 1672 has a large bar which is estimated to measure around 20 kpc.<ref name="Becketal2002">{{Cite journal
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| pages = 83&ndash;102
| pages = 83&ndash;102
| author = Beck, R. |display-authors=4 | author2 = Shoutenkov, V. | author3 = Ehle, M. | author4 = Harnett, J. I. | author5 = Haynes, R. F. | author6 = Shukurov, A. | author7 = Sokoloff, D. D. | author8 = Thierbach, M.
| author = Beck, R. |display-authors=4 | author2 = Shoutenkov, V. | author3 = Ehle, M. | author4 = Harnett, J. I. | author5 = Haynes, R. F. | author6 = Shukurov, A. | author7 = Sokoloff, D. D. | author8 = Thierbach, M.
|arxiv = astro-ph/0207201 | s2cid = 14749261
|arxiv = astro-ph/0207201 }}</ref> It has very strong radio emissions emanating from its nucleus, bar, and the inner portion of the spiral arm region.<ref name="Becketal2002" /> The nucleus is [[Seyfert galaxy#Classification of Seyfert galaxies|Seyfert type 2]] and is engulfed by a [[starburst (astronomy)|starburst]] region.<ref name="Becketal2002" /> The strongest polarized emissions come from the northeastern region which is upstream from its dust lanes.<ref name="Becketal2002" /> Magnetic field lines are at large angles with respect to the bar and turn smoothly to the center.<ref name="Becketal2002" />
}}</ref> It has very strong radio emissions emanating from its nucleus, bar, and the inner portion of the spiral arm region.<ref name="Becketal2002" /> The nucleus is [[Seyfert type II]] and is engulfed by a [[starburst region]].<ref name="Becketal2002" /> The strongest polarized emissions come from the northeastern region which is upstream from its dust lanes.<ref name="Becketal2002" /> Magnetic field lines are at large angles with respect to the bar and turn smoothly to the center.<ref name="Becketal2002" />

Two [[supernova]]e have been observed in NGC 1672: SN 2017gax ([[Type Ib and Ic supernovae|type&nbsp;Ib/c]], mag. 14.1)<ref>[https://www.wis-tns.org/object/2017gax Transient Name Server entry for SN 2017gax.] Retrieved 24 March 2023.</ref> and SN 2022aau ([[Type II supernova|type&nbsp;II]], mag. 16.3).<ref>[https://www.wis-tns.org/object/2022aau Transient Name Server entry for SN 2022aau.] Retrieved 24 March 2023.</ref>


==General structure==
==General structure==
The center of the galaxy contains a high surface brightness bar, and four filament-like [[spiral arm]]s extend outward from the ends of this bar. The spiral arms are asymmetric; one of the arms in the northeast part of the disk is significantly brighter than its counterpart on the other side. The spiral arms also contain numerous [[star formation]] regions, some of which may be as large as {{nowrap|4&prime;&prime;}}.<ref name="carnegieatlas">{{cite book
The center of the galaxy contains a high surface brightness bar, and four filament-like [[spiral arm]]s extend outward from the ends of this bar. The spiral arms are asymmetric; one of the arms in the northeast part of the disk is significantly brighter than its counterpart on the other side. The spiral arms also contain numerous [[star formation]] regions, some of which may be as large as {{pprime|4}}.<ref name="carnegieatlas">{{cite book
| author=A. Sandage | author2= J. Bedke
| author=A. Sandage | author2= J. Bedke
| date=1994
| date=1994
Line 72: Line 76:
| bibcode=1997A&A...319...52V
| bibcode=1997A&A...319...52V
}}</ref>
}}</ref>
*A nuclear HII region, a region which has a spectrum similar to that of [[star formation]] regions in the [[Milky Way]] and which therefore is associated with nuclear star formation activity.
*A nuclear H II region, a region which has a spectrum similar to that of [[star formation]] regions in the [[Milky Way]] and which therefore is associated with nuclear star formation activity.
*A [[Seyfert galaxy|Seyfert nucleus]], a type of [[active galactic nucleus]] (AGN) that may contain a [[supermassive black hole]].
*A [[Seyfert galaxy|Seyfert nucleus]], a type of [[active galactic nucleus]] (AGN) that may contain a [[supermassive black hole]].
*A [[low ionization nuclear emission-line region]], a type of nuclear region with [[spectral line]] emission from weakly [[ion]]ized gas that could contain either a star formation region or a supermassive black hole.
*A [[low-ionization nuclear emission-line region]], a type of nuclear region with [[spectral line]] emission from weakly [[ion]]ized gas that could contain either a star formation region or a supermassive black hole.


NGC 1672, however, is one of several nearby galaxies that does not fit into this classification scheme, as its spectrum appears intermediary between these three classes of objects.<ref name="veron1997"/> It may in fact contain both nuclear star formation regions and an AGN. In some wave bands (such as in [[ultraviolet light]]), the star formation regions are the primary source of emission.<ref name="kinneyetal1993">{{cite journal
NGC 1672, however, is one of several nearby galaxies that does not fit into this classification scheme, as its spectrum appears intermediary between these three classes of objects.<ref name="veron1997"/> It may in fact contain both nuclear star formation regions and an AGN. In some wave bands (such as in [[ultraviolet light]]), the star formation regions are the primary source of emission.<ref name="kinneyetal1993">{{cite journal
Line 84: Line 88:
| pages=5–93
| pages=5–93
| bibcode=1993ApJS...86....5K
| bibcode=1993ApJS...86....5K
| doi=10.1086/191771}}</ref>
| doi=10.1086/191771| doi-access=free}}</ref>


==Gallery==
==Gallery==
Line 90: Line 94:
NGC 1672 HST.jpg | A [[Hubble Space Telescope]] image of the center region of NGC 1672
NGC 1672 HST.jpg | A [[Hubble Space Telescope]] image of the center region of NGC 1672
NGC 1672 GALEX WikiSky.jpg | A [[GALEX]] [[ultraviolet]] image of NGC 1672
NGC 1672 GALEX WikiSky.jpg | A [[GALEX]] [[ultraviolet]] image of NGC 1672
NGC 1672 (weic2403k).jpg | A [[James Webb Space Telescope]] image of NGC 1672
</gallery>
</gallery>


==See also==
==See also==
* [[NGC 1300]]
* [[NGC 1300]]-A barred spiral galaxy.
* [[NGC 7552]]-A very similar-looking barred spiral galaxy.


==References==
==References==
Line 100: Line 106:
==External links==
==External links==
{{commons category|NGC 1672}}
{{commons category|NGC 1672}}
* [http://hubblesite.org/newscenter/archive/releases/2007/15/fastfacts/ Hubblesite Newscenter: Pictures and description]
* [https://hubblesite.org/contents/media/images/2007/15/2092-Image.html Hubblesite Newscenter: Pictures and description]


{{Sky|04|45|42.500|-|59|14|49.85}}
{{Sky|04|45|42.500|-|59|14|49.85}}
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[[Category:Seyfert galaxies]]
[[Category:Seyfert galaxies]]
[[Category:LINER galaxies]]
[[Category:LINER galaxies]]
[[Category:Dorado (constellation)]]
[[Category:Dorado]]
[[Category:NGC objects|1672]]
[[Category:NGC objects|1672]]
[[Category:Principal Galaxies Catalogue objects|15941]]
[[Category:Principal Galaxies Catalogue objects|15941]]

Latest revision as of 11:35, 6 June 2024

NGC 1672
The galaxy photographed with the Víctor M. Blanco Telescope
Observation data (J2000 epoch)
ConstellationDorado
Right ascension04h 45m 42.500s[1]
Declination−59° 14′ 49.85″[1]
Redshift1331 ± 3 km/s[1]
Distance51.7 ± 3.0 Mly (15.86 ± 0.92 Mpc)[2]
Apparent magnitude (V)10.3[1]
Characteristics
Type(R')SB(r)bc[1]
Apparent size (V)6.6′ × 5.5′[1]
Other designations
PGC 15941[1]

NGC 1672 is a barred spiral galaxy located in the constellation Dorado. It was discovered by the astronomer James Dunlop on November 5, 1826.[3] It was originally unclear whether it was a member of the Dorado Group, with some sources[4] finding it to be a member and other sources[5] 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.[2]

NGC 1672 has a large bar which is estimated to measure around 20 kpc.[6] It has very strong radio emissions emanating from its nucleus, bar, and the inner portion of the spiral arm region.[6] The nucleus is Seyfert type II and is engulfed by a starburst region.[6] The strongest polarized emissions come from the northeastern region which is upstream from its dust lanes.[6] Magnetic field lines are at large angles with respect to the bar and turn smoothly to the center.[6]

Two supernovae have been observed in NGC 1672: SN 2017gax (type Ib/c, mag. 14.1)[7] and SN 2022aau (type II, mag. 16.3).[8]

General structure

[edit]

The center of the galaxy contains a high surface brightness bar, and four filament-like spiral arms extend outward from the ends of this bar. The spiral arms are asymmetric; one of the arms in the northeast part of the disk is significantly brighter than its counterpart on the other side. The spiral arms also contain numerous star formation regions, some of which may be as large as 4″.[9]

Nucleus

[edit]

The classification of the nucleus of NGC 1672 is uncertain. Most galaxies may be classified by their spectra as having one of three different types of nuclei:[10]

NGC 1672, however, is one of several nearby galaxies that does not fit into this classification scheme, as its spectrum appears intermediary between these three classes of objects.[10] It may in fact contain both nuclear star formation regions and an AGN. In some wave bands (such as in ultraviolet light), the star formation regions are the primary source of emission.[11]

[edit]

See also

[edit]
  • NGC 1300-A barred spiral galaxy.
  • NGC 7552-A very similar-looking barred spiral galaxy.

References

[edit]
  1. ^ a b c d e f g "Results for object NGC 1672 (NGC 1672)". NASA/IPAC Extragalactic Database. California Institute of Technology. Retrieved 2021-04-29.
  2. ^ a b Tikhonov, N. A.; Galazutdinova, O. A. (2020). "Distance to the Dorado Group". Astrophysical Bulletin. 75 (4): 384–393. arXiv:2009.04090. Bibcode:2020AstBu..75..384T. doi:10.1134/S199034132004015X. S2CID 221556782.
  3. ^ Seligman, Courtney. "New General Catalogue objects: NGC 1650 - 1699". cseligman.com. Retrieved 2021-04-29.
  4. ^ Huchra, J. P.; Geller, M. J. (June 15, 1982). "Groups of galaxies. I - Nearby groups". Astrophysical Journal. 257 (Part 1): 423–437. Bibcode:1982ApJ...257..423H. doi:10.1086/160000.
  5. ^ Maia, M. A. G.; da Costa, L. N.; Latham, David W. (April 1989). "A catalog of southern groups of galaxies". Astrophysical Journal Supplement Series. 69: 809–829. Bibcode:1989ApJS...69..809M. doi:10.1086/191328. ISSN 0067-0049.
  6. ^ a b c d e Beck, R.; Shoutenkov, V.; Ehle, M.; Harnett, J. I.; et al. (August 2002). "Magnetic fields in barred galaxies. I. The atlas". Astronomy and Astrophysics. 391 (1): 83–102. arXiv:astro-ph/0207201. Bibcode:2002A&A...391...83B. doi:10.1051/0004-6361:20020642. S2CID 14749261.
  7. ^ Transient Name Server entry for SN 2017gax. Retrieved 24 March 2023.
  8. ^ Transient Name Server entry for SN 2022aau. Retrieved 24 March 2023.
  9. ^ A. Sandage; J. Bedke (1994). Carnegie Atlas of Galaxies. Washington, D.C.: Carnegie Institution of Washington. ISBN 978-0-87279-667-6.
  10. ^ a b P. Veron; A. C. Goncalves; M. P. Veron-Cetty (1997). "AGNs with composite spectra". Astronomy and Astrophysics. 319: 52–66. Bibcode:1997A&A...319...52V.
  11. ^ A. L. Kinney; R. C. Bohlin; D. Calzetti; N. Panagia; et al. (1993). "An atlas of ultraviolet spectra of star-forming galaxies". Astrophysical Journal Supplement Series. 86: 5–93. Bibcode:1993ApJS...86....5K. doi:10.1086/191771.
[edit]
Wikimedia Commons has media related to NGC 1672.


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