NGC 5377 is an intermediate barred spiral galaxy located in the constellation Canes Venatici. Its speed relative to the cosmic microwave background is 1,951 ± 11 km/s, which corresponds to a Hubble distance of 28.8 ± 2.0 Mpc (∼93.9 million ly).[1] NGC 5377 was discovered by German-British astronomer William Herschel in 1787.
| NGC 5377 | |
|---|---|
 NGC 5377 imaged by the Hubble Space Telescope | |
| Observation data (J2000 epoch) | |
| Constellation | Canes Venatici |
| Right ascension | 13h 56m 17s |
| Declination | +47° 14’ 08” |
| Redshift | 0.005991 |
| Heliocentric radial velocity | 1,796 km/s |
| Distance | 93.9 Mly (28.78 kpc) |
| Apparent magnitude (V) | 11.46 |
| Apparent magnitude (B) | 12.39 |
| Surface brightness | 23.29 mag/arcsec^2 |
| Characteristics | |
| Type | (R)SB(s)a |
| Size | 111,000 ly (33.93 kpc) |
| Apparent size (V) | 4.7' x 2.4' |
| Other designations | |
| PGC 49563, UGC 8863, KARA 604, MCG +08-25-052, CGCG 246-027, IRAS 13542+4729 | |
NGC 5377 was used by Gérard de Vaucouleurs as a morphological type galaxy SAb in his galaxy atlas.[2][3]
The luminosity class of NGC 5377 is I and it has a broad HI line. NGC 5377 also has an active galactic nucleus.[1]
To date, 17 non-redshift measurements yield a distance of 25.918 ± 5.770 Mpc (∼84.5 million ly),[4] which is within the Hubble distance range. Note, however, that it is with the average value of independent measurements, when they exist, that the NASA/IPAC database calculates the diameter of a galaxy and that consequently the diameter of NGC 5377 could be approximately 37.7 kpc (∼123,000 ly) if Hubble distance is used to calculate it.
Nucleic disk
editWith observations from the Hubble Space Telescope, a star-forming disk was observed around the core of NGC 5377. The size of its semi-major axis is estimated at 790 pc (~2,575 light years).[5]
Supermassive black hole
editAccording to a study based on near-infrared K-band luminosity measurements of the nuclei of NGC 5377, a supermassive black hole with an apparent mass of approximately 107.8 𝑀⊙ (63 million solar masses) exists within the core of the galaxy.[6]
Supernova
editSupernova SN 1992H (type II, mag. 15)[7] was discovered on February 11, 1992, by William R. Wren of the McDonald Observatory at the University of Texas at Austin.[8]
NGC 5448 group
editNGC 5377 is a member of the NGC 5448 Group according to A.M. Garcia. The group has nine galaxies, including NGC 5425, NGC 5448, NGC 5481, NGC 5500, NGC 5520, UGC 9056 and UGC 9083.[9]
See also
editExternal links
editReferences
edit- ^ a b "By Name | NASA/IPAC Extragalactic Database". ned.ipac.caltech.edu. Retrieved 2024-07-24.
- ^ "Gérard de Vaucouleurs' Atlas of Galaxies". cseligman.com. Retrieved 2024-07-24.
- ^ "The Galaxy Morphology Website, NGC 5377". kudzu.astr.ua.edu. Retrieved 2024-07-24.
- ^ "NED Query Results for NGC 5375". ned.ipac.caltech.edu. Retrieved 2024-07-24.
- ^ Comeron, S.; Knapen, J. H.; Beckman, J. E.; Laurikainen, E.; Salo, H.; Martinez-Valpuesta, I.; Buta, R. J. (November 1, 2018). "AINUR: Atlas of Images of NUclear Rings". ArXiv. Retrieved July 23, 2024.
- ^ "Other Supernovae images". rochesterastronomy.org. Retrieved 2024-07-24.
- ^ Transient Name Server entry for SN 1992H. Retrieved 23 July 2024.
- ^ Clocchiatti, Alejandro; Benetti, Stefano; Wheeler, J. Craig; Wren, William; Boisseau, J.; Cappellaro, Enrico; Turatto, Massimo; Patat, Ferdinando; Swartz, Douglas A.; Harkness, Robert P.; Brotherton, Michael S.; Wills, Beverly; Hemenway, Paul; Cornell, Mark; Frueh, Marian (1996-03-01). "A Study of SN 1992H in NGC 5377". The Astronomical Journal. 111: 1286. doi:10.1086/117874. ISSN 0004-6256.
- ^ Garcia, A. M. (1993-07-01). "General study of group membership. II. Determination of nearby groups". Astronomy and Astrophysics Supplement Series. 100: 47–90. ISSN 0365-0138.