Astronomy:NGC 5238

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Short description: Galaxy in constellation Canes Venatici
NGC 5238
NGC 5238 Hubble WikiSky.jpg
Hubble Space Telescope image of NGC 5238
Observation data (J2000 epoch)
ConstellationCanes Venatici
Right ascension 13h 34m 43.8s[1]
Declination+51° 36′ 33″[1]
Redshift0.0015[2]
Helio radial velocity229 km/s[3]
Distance4.51 Mpc[4]
Characteristics
Mass/Light ratio0.6[5] M☉/L☉
Apparent size (V)64.4"[6]
Other designations
UGC 8565, VV 828, Mrk 1479, SBS 1332+518, I Zw 64, KPG 384

NGC 5238 is an irregular galaxy[7] in the constellation Canes Venatici. Located at a comoving distance of 4.51 Mpc,[4] it is 64.4 arcseconds in diameter.[6] It has sometimes been classified as a blue compact dwarf galaxy.[8] Although some authors have hypothesized it to be a member of the M101 Group of galaxies, it is currently believed to be an isolated galaxy.[9]

At an inclination of 39° with respect to Earth,[3] NGC 5238 has a total mass of 117 million solar masses,[10] with a star formation rate of 0.01 solar masses per year.[11] Of the total mass, HI gas appears to account for 26 million solar masses.[3]

Classification

In 1977, NGC 5238 was hypothesized to not be a single galaxy, but rather a pair of interacting galaxies.[12] It was not until ten years later that a dedicated study of the galaxy's rotation curve was undertaken, showing that the galaxy is indeed a single galaxy. One of the two regions that was thought to be the nucleus of a galaxy was instead shown to be simply a large HII region around 100 pc in diameter.[13]

The morphological type of NGC 5238 has been the subject of some controversy. In 1979, the galaxy was classified as a barred spiral galaxy.[14] Soon after, in 1984, the galaxy was included in a study of blue compact dwarf galaxies, incompatible with the classification of a barred spiral.[15] However, the barred spiral classification was considered the correct classification for years. It was not until the mid 1990s that the galaxy was first recognized as a dwarf irregular galaxy.[16][17] Even after this, the majority of studies recognized the galaxy as a spiral galaxy until 2015, when the classification of irregular finally became widely accepted[7][8]

Appearance

As it appears to us, NGC 5238 is tilted at an inclination of 39°.[3] This 2013 estimate follows previous estimates of 30° in 1987,[13] 37 ± 5° in 1992,[18] and 47° in 1999[19] In the Spitzer 3.6 µm band, the semimajor axis of its angular size is 64.4", with an ellipticity of 0.201.[6]

Distance

The distance estimate to NGC 5238 has been brought down considerably since first calculated. The first published distance estimate was 7 Mpc, derived using redshift.[14] This remained the predominant estimate until 1996, when the distance was found to be much less, estimated at 5.18 Mpc.[20] Subsequently, using spectral data from the HI 21cm line, the distance was calculated to be 4.7 Mpc in 1999,[21] although an updated HI study found a slightly higher value at 5.20 Mpc in 2002.[22] Five years later, in 2007, the distance estimate was lowered even further to 4.50 Mpc, extremely close to today's accepted value.[23]

One way to determine distance unambiguously is by standard candles. The tip of the red giant branch is such a method; every galaxy's brightest red giant stars must have exactly the same known luminosity. When combined with corrections for interstellar reddening, this allows for accurate determination of a galaxy's distance. By 2009, a Hubble Space Telescope image of NGC 5238 had become available, resolving the individual stars within the galaxy. Using this method, the distance modulus was calculated at 28.27 magnitudes, corresponding to a distance of 4.51 Mpc, today's accepted value.[4]

Radio emission

Since a first study was published in 1986, the neutral hydrogen gas of NGC 5238 and its associated 21 cm line have been the subject of many studies. The first study calculated the total HI 21 cm flux from the galaxy to be 4.5 ± 1.0 Jy·km/s, with a full width at half maximum of 28 km/s and a maximum flux density of 0.25 ± 0.011 Jy.[24] Two years later, the 20% line width was calculated at two conflicting values from two studies: 47 km/s and 65 km/s.[5][25] From the HI line data, the total mass to HI mass ratio was calculated to be 0.384 and the pseudo HI surface density was estimated to be 9.7 solar masses per square parsec.[5] Another two years later, another estimate for the 20% and 50% line widths was published, calculating 36 ± 4 km/s at 50% and 49 ± 4 at 20%.[26]

In 1999, the 50% line width was further refined to 32 ± 4 km/s,[21] then 36 km/s. The second study, in addition to deriving the 5.20 Mpc distance quoted above, found a total HI mass of 4.2×107 solar masses.[22] Finally, in 2013, the 50% line width estimate was further increased to 40 km/s, and the HI mass was refined to 2.6×107 solar masses, implying a total-to-HI mass ratio of 7.3.[3]

In addition to HI gas, it is thought that radio continuum emission should be present from NGC 5238 as well. The galaxy is a strong ultraviolet emitter, indicating that the galaxy is undergoing rapid star formation. Based on this, it is to be expected that there should be radio continuum emission from the galaxy, due to the acceleration of electrons in HII regions, known as bremsstrahlung. However, such emission has not been found in NGC 5238, contradicting models. To resolve this mystery, it has been hypothesized that the star formation has subsided recently enough that the UV excess from massive stars is still present, but the hydrogen has already recombined.[27]

References

  1. ↑ 1.0 1.1 Paturel, G.; Petit, C.; Prugniel, Ph.; Theureau, G.; Rousseau, J.; Brouty, M.; Dubois, P.; Cambrésy, L. (2003). "HYPERLEDA. I. Identification and designation of galaxies". Astronomy and Astrophysics 412: 45–55. doi:10.1051/0004-6361:20031411. Bibcode: 2003A&A...412...45P. 
  2. ↑ Gyulzadyan, M. V.; Stepanian, J. A.; Petrosian, A. R.; Kunth, D.; McLean, B.; Comte, G. (2003). "Spectroscopic Study of a Large Sample of Galaxies Discovered in the Second Byurakan Survey Fields". Astrophysics (English Translation of Astrofizika) 46 (2): 131. doi:10.1023/A:1024011318696. Bibcode: 2003Ap.....46..131G. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 Karachentsev, Igor D.; Makarov, Dmitry I.; Kaisina, Elena I. (2013). "Updated Nearby Galaxy Catalog". The Astronomical Journal 145 (4): 101. doi:10.1088/0004-6256/145/4/101. Bibcode: 2013AJ....145..101K. 
  4. ↑ 4.0 4.1 4.2 Jacobs, Bradley A.; Rizzi, Luca; Tully, R. Brent; Shaya, Edward J.; Makarov, Dmitry I.; Makarova, Lidia (2009). "The Extragalactic Distance Database: Color-Magnitude Diagrams". The Astronomical Journal 138 (2): 332. doi:10.1088/0004-6256/138/2/332. Bibcode: 2009AJ....138..332J. 
  5. ↑ 5.0 5.1 5.2 Huchtmeier, W. K.; Richter, O.-G. (1988). "H I observations of galaxies in the Kraan-Korteweg-Tammann catalogue of nearby galaxies. III - Global parameters of the galaxies". Astronomy and Astrophysics 203: 237. Bibcode: 1988A&A...203..237H. 
  6. ↑ 6.0 6.1 6.2 Sheth, Kartik; Regan, Michael; Hinz, Joannah L.; Gil De Paz, Armando; Menéndez-Delmestre, Karín; Muñoz-Mateos, Juan-Carlos; Seibert, Mark; Kim, Taehyun et al. (2010). "The Spitzer Survey of Stellar Structure in Galaxies (S4G)". Publications of the Astronomical Society of the Pacific 122 (898): 1397. doi:10.1086/657638. Bibcode: 2010PASP..122.1397S. 
  7. ↑ 7.0 7.1 Cite error: Invalid <ref> tag; no text was provided for refs named Irregular
  8. ↑ 8.0 8.1 Ann, H. B.; Seo, Mira; Ha, D. K. (2015). "A Catalog of Visually Classified Galaxies in the Local (z ∼ 0.01) Universe". The Astrophysical Journal Supplement Series 217 (2): 27. doi:10.1088/0067-0049/217/2/27. Bibcode: 2015ApJS..217...27A. 
  9. ↑ Tikhonov, N. A.; Lebedev, V. S.; Galazutdinova, O. A. (2015). "M 101 group galaxies". Astronomy Letters 41 (6): 239. doi:10.1134/S1063773715060080. Bibcode: 2015AstL...41..239T. 
  10. ↑ Cite error: Invalid <ref> tag; no text was provided for refs named mass
  11. ↑ Karachentsev, Igor D.; Kaisina, Elena I. (2013). "Star Formation Properties in the Local Volume Galaxies via Hα and Far-ultraviolet Fluxes". The Astronomical Journal 146 (3): 46. doi:10.1088/0004-6256/146/3/46. Bibcode: 2013AJ....146...46K. 
  12. ↑ Vorontsov-Velyaminov, B. A. (1977). "Atlas of interacting galaxies, part II and the concept of fragmentation of galaxies". Astronomy and Astrophysics 28: 1. Bibcode: 1977A&AS...28....1V. 
  13. ↑ 13.0 13.1 Arkhipova, V. P.; Noskova, R. I.; Sil'Chenko, O. K.; Zasov, A. V. (1987). "The internal motions in three dwarf irregular galaxies". Pis'ma v Astronomicheskii Zhurnal 13: 575. Bibcode: 1987PAZh...13..575A. 
  14. ↑ 14.0 14.1 Kraan-Korteweg, R. C.; Tammann, G. A. (1979). "A catalogue of galaxies within 10 MPC". Astronomische Nachrichten 300 (4): 181. doi:10.1002/asna.19793000403. Bibcode: 1979AN....300..181K. 
  15. ↑ Klein, U.; Wielebinski, R.; Thuan, T. X. (1984). "Radio continuum observations of blue compact dwarf galaxies". Astronomy and Astrophysics 141: 241. Bibcode: 1984A&A...141..241K. 
  16. ↑ Karachentsev, I. D.; Tikhonov, N. A. (1994). "New photometric distances for dwarf galaxies in the Local Volume". Astronomy and Astrophysics 286: 718. Bibcode: 1994A&A...286..718K. 
  17. ↑ Han, Cheongho; Gould, Andrew; Sackett, Penny D. (1995). "The Orientation of Spin Vectors of Galaxies in the Ursa Major Filament". The Astrophysical Journal 445: 46. doi:10.1086/175671. Bibcode: 1995ApJ...445...46H. 
  18. ↑ Schmidt, K.-H.; Boller, T. (1992). "Nearby galaxies. I - the catalogue". Astronomische Nachrichten 313 (4): 189. doi:10.1002/asna.2113130402. Bibcode: 1992AN....313..189S. 
  19. ↑ Bremnes, T.; Binggeli, B.; Prugniel, P. (1999). "Structure and stellar content of dwarf galaxies. III. B and R photometry of dwarf galaxies in the M 101 group and the nearby field". Astronomy and Astrophysics Supplement 137 (2): 337. doi:10.1051/aas:1999486. Bibcode: 1999A&AS..137..337B. 
  20. ↑ Karachentsev, I. D.; Makarov, D. A. (1996). "The Galaxy Motion Relative to Nearby Galaxies and the Local Velocity Field". Astronomical Journal 111: 794. doi:10.1086/117825. Bibcode: 1996AJ....111..794K. 
  21. ↑ 21.0 21.1 Thuan, Trinh X.; Lipovetsky, V. A.; Martin, J.-M.; Pustilnik, S. A. (1999). "HI observations of blue compact galaxies from the first and second Byurakan surveys". Astronomy and Astrophysics Supplement 139: 1–24. doi:10.1051/aas:1999373. Bibcode: 1999A&AS..139....1T. 
  22. ↑ 22.0 22.1 Swaters, R. A.; Balcells, M. (2002). "The Westerbork HI survey of spiral and irregular galaxies. II. R-band surface photometry of late-type dwarf galaxies". Astronomy and Astrophysics 390 (3): 863. doi:10.1051/0004-6361:20020449. Bibcode: 2002A&A...390..863S. 
  23. ↑ Lira, P.; Johnson, R. A.; Lawrence, A.; Cid Fernandes, R. (2007). "Multiwavelength study of the nuclei of a volume-limited sample of galaxies - II. Optical, infrared and radio observations". Monthly Notices of the Royal Astronomical Society 382 (4): 1552. doi:10.1111/j.1365-2966.2007.12006.x. Bibcode: 2007MNRAS.382.1552L. http://repositorio.uchile.cl/bitstream/handle/2250/126071/Lira_P_Multiwavelength.pdf?sequence=1&isAllowed=y. 
  24. ↑ Huchtmeier, W. K.; Richter, O. G. (1986). "HI-observations of galaxies in the Kraan-Korteweg - Tammann catalogue of nearby galaxies. I - the data". Astronomy and Astrophysics Supplement Series 63: 323. Bibcode: 1986A&AS...63..323H. 
  25. ↑ Tifft, W. G.; Cocke, W. J. (1988). "Uncertainties in 21 centimeter redshifts. I - Data". Astrophysical Journal Supplement Series 67: 1. doi:10.1086/191265. Bibcode: 1988ApJS...67....1T. 
  26. ↑ Bottinelli, L.; Gouguenheim, L.; Fouque, P.; Paturel, G. (1990). "An extragalactic data base. II - the HI data". Astronomy and Astrophysics Supplement Series 82: 391. Bibcode: 1990A&AS...82..391B. 
  27. ↑ Aversa, Alan G.; Johnson, Kelsey E.; Brogan, Crystal L.; Goss, W. M.; Pisano, D. J. (2011). "Very Large Array and ATCA Search for Natal Star Clusters in Nearby Star-forming Galaxies". The Astronomical Journal 141 (4): 125. doi:10.1088/0004-6256/141/4/125. Bibcode: 2011AJ....141..125A. 

External links

Coordinates: Sky map 13h 37m 00.9s, −29° 51′ 57″



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