NGC 7418

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NGC 7418
NGC 7418 hst 08599 814.png
NGC 7418 by Hubble Space Telescope
Observation data (J2000 epoch)
Constellation Grus
Right ascension 22h 56m 36.2s [1]
Declination −37° 01′ 48.3″ [1]
Redshift 0.004837 ± 0.000017 [1]
Helio radial velocity 1,450 ± 5 km/s [1]
Distance 59.1 ± 8.5 Mly (18.2 ± 2.6 Mpc) [1]
Apparent magnitude  (V)11.0
Characteristics
Type SAB(rs)cd [1]
Apparent size  (V)3.5′ × 2.6′ [1]
Other designations
ESO 406- G025, MCG -06-50-013, PGC 70069 [1]

NGC 7418 is an intermediate spiral galaxy located in the constellation Grus. It is located at a distance of circa 60 million light-years from Earth, which, given its apparent dimensions, means that NGC 7418 is about 60,000 light-years across. [1] It was discovered by John Herschel on August 30, 1834. [2]

Contents

Characteristics

NGC 7418 has a bright nucleus incorporated into a bar. The bar appears strong in the infrared H-band while in the optical wavelengths it appears weaker or even unbarred. The spiral arms of the galaxy emanate from the end of the bar. The galaxy has four grand design spiral arms. Their inner parts have knots while the outermost are smooth. [3] The galaxy is seen with an inclination of 42 degrees. [4]

In the centre of NGC 7418 is believed to lie a supermassive black hole with an estimated mass between 1 and 15 million (106.58 ± 0.59) M☉, based on the spiral pitch angle. [5] The centre of the galaxy has also been found to host a massive stellar cluster, with an estimated mass of nearly 60 million (107.78 ± 0.19) M☉. [6] The existence of this nuclear star cluster doesn't rule out the existence of a supermassive black hole. Galaxies like the Milky Way and the Andromeda Galaxy have been found to host both. [5] The stellar population at the nucleus of NGC 7418 has been found to be quite young, with mean age less than 100 million years, indicating recent star forming activity. [7]

One supernova has been observed in NGC 7418, SN 1983 Z. It was discovered by L. E. Gonzalez at Cerro El Roble 11" west and 52" south of the nucleus. On September 3, 1983 it had an apparent magnitude of 15.5. [8]

Nearby galaxies

NGC 7418 is a member of a galaxy group known as the IC 1459 group. It is a loose group centred at IC 1459 and contains a large number of spiral galaxies. [9] Other members include NGC 7418A, NGC 7421, IC 5264, IC 5269, IC 5269B, IC 5270, and IC 5273. [10] NGC 7421 lies 19.5 arcminutes away and NGC 7418A lies 16.5 arcminutes to the north as seen in the sky. [11] This group, along with the NGC 7582 group, form the Grus cloud, a region of elevated galaxy density. [9] The Grus cloud, along with the nearby Pavo-Indus cloud, lies between the Local Supercluster and Pavo–Indus Supercluster. [12]

The group features both diffuse X-ray emission from the intergalactic medium and HI emission. Based on the presence of both, it has been suggested that the group is in its early stages of assembling from different subgroups. Three HI clouds have been found to be associated with the group, two located near IC 5270 and one near NGC 7418, at its northwest edge, with total mass 6×108 M☉. These HI clouds are believed to have formed from gas stripped from the galaxies as a result of interactions. [9]

NGC 7418 (HST - Aladin software) NGC7418-hst-814.png
NGC 7418 (HST - Aladin software)

Related Research Articles

<span class="mw-page-title-main">Grus (constellation)</span> Constellation in the southern celestial hemisphere

Grus is a constellation in the southern sky. Its name is Latin for the crane, a type of bird. It is one of twelve constellations conceived by Petrus Plancius from the observations of Pieter Dirkszoon Keyser and Frederick de Houtman. Grus first appeared on a 35-centimetre-diameter (14-inch) celestial globe published in 1598 in Amsterdam by Plancius and Jodocus Hondius and was depicted in Johann Bayer's star atlas Uranometria of 1603. French explorer and astronomer Nicolas-Louis de Lacaille gave Bayer designations to its stars in 1756, some of which had been previously considered part of the neighbouring constellation Piscis Austrinus. The constellations Grus, Pavo, Phoenix and Tucana are collectively known as the "Southern Birds".

<span class="mw-page-title-main">Local Group</span> Group of galaxies that includes the Milky Way

The Local Group is the galaxy group that includes the Milky Way. It has a total diameter of roughly 3 megaparsecs (10 million light-years; 9×1019 kilometres), and a total mass of the order of 2×1012 solar masses (4×1042 kg). It consists of two collections of galaxies in a "dumbbell" shape; the Milky Way and its satellites form one lobe, and the Andromeda Galaxy and its satellites constitute the other. The two collections are separated by about 800 kiloparsecs (3×10^6 ly; 2×1019 km) and are moving toward one another with a velocity of 123 km/s. The group itself is a part of the larger Virgo Supercluster, which may be a part of the Laniakea Supercluster. The exact number of galaxies in the Local Group is unknown as some are occluded by the Milky Way; however, at least 80 members are known, most of which are dwarf galaxies.

<span class="mw-page-title-main">NGC 1569</span> Galaxy in the constellation Camelopardalis

NGC 1569 is a dwarf irregular galaxy in Camelopardalis. The galaxy is relatively nearby and consequently, the Hubble Space Telescope can easily resolve the stars within the galaxy. The distance to the galaxy was previously believed to be only 2.4 Mpc. However, in 2008 scientists studying images from Hubble calculated the galaxy's distance at nearly 11 million light-years away, about 4 million light-years farther than previous thought, meaning it is a member of the IC 342 group of galaxies.

The Pavo–Indus Supercluster is a neighboring supercluster located about 60–70 Mpc (196–228 Mly) away in the constellations of Pavo, Indus, and Telescopium. The supercluster contains three main clusters, Abell 3656, Abell 3698, and Abell 3742.

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

The Dorado Group is a loose concentration of galaxies containing both spirals and ellipticals. It is generally considered a 'galaxy group' but may approach the size of a 'galaxy cluster'. It lies primarily in the southern constellation Dorado and is one of the richest galaxy groups of the Southern Hemisphere. Gérard de Vaucouleurs was the first to identify it in 1975 as a large complex nebulae II in the Dorado region, designating it as G16.

<span class="mw-page-title-main">NGC 7424</span> Galaxy in the constellation Grus

NGC 7424 is a barred spiral galaxy located 37.5 million light-years away in the southern constellation Grus. Its size makes it similar to our own galaxy, the Milky Way. It is called a "grand design" galaxy because of its well defined spiral arms. Two supernovae and two ultraluminous X-ray sources have been discovered in NGC 7424.

<span class="mw-page-title-main">NGC 672</span> Galaxy in the constellation Triangulum

NGC 672 is a spiral galaxy in the northern constellation of Triangulum, positioned around 2° to the southwest of the star Alpha Trianguli. The original object designated NGC 672 was discovered by the German-born astronomer William Herschel on 26 October 1786, but this was later cataloged as NGC 614. The object now identified as NGC 672 was discovered by John Herschel on 11 November 1827.

<span class="mw-page-title-main">NGC 7552</span> Galaxy in the constellation Grus

NGC 7552 is a barred spiral galaxy in the constellation Grus. It is at a distance of circa 60 million light years from Earth, which, given its apparent dimensions, means that NGC 7552 is about 75,000 light years across. It forms with three other spiral galaxies the Grus Quartet.

<span class="mw-page-title-main">NGC 1964</span> Galaxy in the constellation Lepus

NGC 1964 is a barred spiral galaxy in the constellation Lepus. The galaxy lies 65 million light years away from Earth, which means, given its apparent dimensions, that NGC 1964 is approximately 100,000 light years across. At its center lies a supermassive black hole, with estimated mass 2.5 × 107M☉. The galaxy features two tightly wound inner spiral arms within a disk with high surface brightness and two outer, more open spiral arms that originate near the inner ring. The outer arms feature few small HII regions.

<span class="mw-page-title-main">Coma I</span> Galaxy cluster in constellation Coma Berenices

The Coma I Group is a group of galaxies located about 14.5 Mpc (47.3 Mly) away in the constellation Coma Berenices. The brightest member of the group is NGC 4725. The Coma I Group is rich in spiral galaxies while containing few elliptical and lenticular galaxies. Coma I lies in the foreground of the more distant Coma and Leo clusters and is located within the Virgo Supercluster.

<span class="mw-page-title-main">NGC 7606</span> Galaxy in the constellation Aquarius

NGC 7606 is a spiral galaxy located in the constellation Aquarius. It is located at a distance of circa 100 million light years from Earth, which, given its apparent dimensions, means that NGC 7606 is about 165,000 light years across. It was discovered by William Herschel on September 28, 1785. The galaxy is included in the Herschel 400 Catalogue. It lies 45 arcminutes northeast from psi2 Aquarii. It can be seen with a 4 inch telescope but its visibility is greatly affected by light pollution.

<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 7213</span> Galaxy in the constellation Grus

NGC 7213 is a lenticular galaxy located in the constellation Grus. It is located at a distance of circa 70 million light-years from Earth, which, given its apparent dimensions, means that NGC 7213 is about 75,000 light-years across. It was discovered by John Herschel on September 30, 1834. It is an active galaxy with characteristics between a type I Seyfert galaxy and LINER.

<span class="mw-page-title-main">NGC 7130</span> Galaxy in the constellation Piscis Austrinus

NGC 7130 is a spiral galaxy located in the constellation Piscis Austrinus. It is located at a distance of about 220 million light years from Earth, which, given its apparent dimensions, means that NGC 7130 is about 100,000 light years across. It was discovered by John Herschel on September 25, 1834, and discovered independently by Lewis Swift on September 17, 1897. The location of the galaxy given in the New General Catalogue was off by 30 arcminutes in declination from the location of the galaxy.

<span class="mw-page-title-main">NGC 3511</span> Galaxy in the constellation Crater

NGC 3511 is an intermediate spiral galaxy located in the constellation Crater. It is located at a distance of circa 45 million light years from Earth, which, given its apparent dimensions, means that NGC 3511 is about 70,000 light years across. It was discovered by William Herschel on December 21, 1786. It lies two degrees west of Beta Crateris.

<span class="mw-page-title-main">NGC 7531</span> Galaxy in the constellation Grus

NGC 7531 is an intermediate spiral galaxy located in the constellation Grus. It is located at a distance of circa 70 million light-years from Earth, which, given its apparent dimensions, means that NGC 7531 is about 95,000 light years across. It was discovered by John Herschel on September 2, 1836.

<span class="mw-page-title-main">IC 1459</span> Elliptical galaxy in the constellation of Grus

IC 1459 is an elliptical galaxy located in the constellation Grus. It is located at a distance of circa 85 million light-years from Earth, which, given its apparent dimensions, means that IC 1459 is about 130,000 light-years across. It was discovered by Edward Emerson Barnard in 1892.

<span class="mw-page-title-main">NGC 4278</span> Galaxy in the constellation Coma Berenices

NGC 4278 is an elliptical galaxy located in the constellation Coma Berenices. It is located at a distance of circa 55 million light years from Earth, which, given its apparent dimensions, means that NGC 4278 is about 65,000 light years across. It was discovered by William Herschel on March 13, 1785. NGC 4278 is part of the Herschel 400 Catalogue and can be found about one and 3/4 of a degree northwest of Gamma Comae Berenices even with a small telescope.

<span class="mw-page-title-main">NGC 5363</span> Galaxy in the constellation Virgo

NGC 5363 is a lenticular galaxy located in the constellation Virgo. It is located at a distance of circa 65 million light years from Earth, which, given its apparent dimensions, means that NGC 5363 is about 100,000 light years across. It was discovered by William Herschel on January 19, 1784. It is a member of the NGC 5364 Group of galaxies, itself one of the Virgo III Groups strung out to the east of the Virgo Supercluster of galaxies.

<span class="mw-page-title-main">NGC 4393</span> Galaxy in the constellation of Coma Berenices

NGC 4393 is a spiral galaxy about 46 million light-years away in the constellation Coma Berenices. It was discovered by astronomer William Herschel on April 11, 1785. It is a member of the NGC 4274 Group, which is part of the Coma I Group or Cloud.

References

  1. 1 2 3 4 5 6 7 8 9 "NASA/IPAC Extragalactic Database". Results for NGC 7418. Retrieved 2019-01-18.
  2. ↑ Seligman, Courtney. "NGC 7418 (= PGC 70069)". Celestial Atlas. Retrieved 19 November 2018.
  3. ↑ Eskridge, Paul B.; Frogel, Jay A.; Pogge, Richard W.; Quillen, Alice C.; Berlind, Andreas A.; Davies, Roger L.; DePoy, D. L.; Gilbert, Karoline M.; Houdashelt, Mark L.; Kuchinski, Leslie E.; Ramirez, Solange V.; Sellgren, K.; Stutz, Amelia; Terndrup, Donald M.; Tiede, Glenn P. (November 2002). "Near-Infrared and Optical Morphology of Spiral Galaxies". The Astrophysical Journal Supplement Series. 143 (1): 73–111. arXiv: astro-ph/0206320 . Bibcode:2002ApJS..143...73E. doi:10.1086/342340. S2CID   15491635.
  4. ↑ Munoz-Mateos, J. C.; Gil de Paz, A.; Boissier, S.; Zamorano, J.; Jarrett, T.; Gallego, J.; Madore, B. F. (April 2007). "Specific Star Formation Rate Profiles in Nearby Spiral Galaxies: Quantifying the Inside-Out Formation of Disks". The Astrophysical Journal. 658 (2): 1006–1026. arXiv: astro-ph/0612017 . Bibcode:2007ApJ...658.1006M. doi:10.1086/511812. S2CID   41735449.
  5. 1 2 Davis, Benjamin L.; Berrier, Joel C.; Johns, Lucas; Shields, Douglas W.; Hartley, Matthew T.; Kennefick, Daniel; Kennefick, Julia; Seigar, Marc S.; Lacy, Claud H. S. (20 June 2014). "The Black Hole Mass Function Derived from Local Spiral Galaxies". The Astrophysical Journal. 789 (2): 124. arXiv: 1405.5876 . Bibcode:2014ApJ...789..124D. doi:10.1088/0004-637X/789/2/124. S2CID   119302157.
  6. ↑ Walcher, C. J.; van der Marel, R. P.; McLaughlin, D.; Rix, H.-W.; Boker, T.; Haring, N.; Ho, L. C.; Sarzi, M.; Shields, J. C. (January 2005). "Masses of Star Clusters in the Nuclei of Bulgeless Spiral Galaxies". The Astrophysical Journal. 618 (1): 237–246. arXiv: astro-ph/0409216 . Bibcode:2005ApJ...618..237W. doi:10.1086/425977. S2CID   14365007.
  7. ↑ Walcher, C. J.; Boker, T.; Charlot, S.; Ho, L. C.; Rix, H.-W.; Rossa, J.; Shields, J. C.; van der Marel, R. P. (October 2006). "Stellar Populations in the Nuclei of Late-Type Spiral Galaxies". The Astrophysical Journal. 649 (2): 692–708. arXiv: astro-ph/0604138 . Bibcode:2006ApJ...649..692W. doi:10.1086/505166. S2CID   18882700.
  8. ↑ "Circular No. 3867". International Astronomical Union Circular. Central Bureau for Astronomical Telegrams. 23 September 1983.
  9. 1 2 3 Serra, P.; et al. (25 July 2015). "ASKAP H i imaging of the galaxy group IC 1459". Monthly Notices of the Royal Astronomical Society. 452 (3): 2680–2691. arXiv: 1506.04399 . Bibcode:2015MNRAS.452.2680S. doi:10.1093/mnras/stv1326.
  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. Archived from the original on 31 January 2016. Retrieved 30 January 2019.
  11. ↑ de Vaucouleurs, G.; de Vaucouleurs, A.; Corwin, J. R. (1976). "Second reference catalogue of bright galaxies". Second Reference Catalogue of Bright Galaxies. 1976. Bibcode:1976RC2...C......0D.
  12. ↑ Fouque, P.; Proust, D.; Quintana, H.; Ramirez, A.; Proust, D.; Quintana, H.; Ramirez, A. (1993). "Dynamics of the Pavo-Indus and Grus Clouds of Galaxies" (PDF). Astronomy and Astrophysics Supplement Series. 100 (3): 493–500. Bibcode:1993A&AS..100..493F.{{cite journal}}: CS1 maint: multiple names: authors list (link)
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