Messier Index/M74

Messier 74 350px Messier 74. Credit: NASA/HST. w:J2000 PiscesR. W. Sinnott, editor The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters by J. L. E. Dreyer 1988 Sky Publishing Corporation and Cambridge University Press 0-933-34651-4 SA(s)c 01 36 41.8 +15 47 01 30 ± 6 Mly 657 km/s 10.0 10′.5 × 9′.5 NGC 628, UGC 1149, PGC 5974 Messier 74 (also known as NGC 628) is a face-on w:spiral galaxy in the w:constellation Pisces. The galaxy contains two clearly-defined w:spiral arms and is therefore used as an archetypal example of a w:Grand Design Spiral Galaxy.A. Sandage, J. Bedke 1994 Carnegie Atlas of Galaxies Carnegie Institution of Washington Washington, D.C. 0-87279-667-1 The galaxy's low surface brightness makes it the most difficult Messier object for amateur astronomers to observe.S. J. O'Meara 1998 The Messier Objects Cambridge University Cambridge 0-521-55332-6K. G. Jones 1991 Messier's Nebulae and Star Clusters 2nd Cambridge University Press Cambridge 0-521-37079-5 However, the relatively large angular size of the galaxy and the galaxy's face-on orientation make it an ideal object for professional astronomers who want to study w:spiral arm structure and spiral density waves. History M74 was discovered by w:Pierre Méchain in w:1780. Méchain then communicated his discovery to w:Charles Messier, who listed the galaxy in his catalog. Supernovae Two w:supernovae have been identified in M74:NASA/IPAC Extragalactic Database Results for NGC 628 http://nedwww.ipac.caltech.edu/ 2006-08-12 2006-08-12 w:SN 2002apS. Nakano, R. Kushida, Y. Kushida, W. Li Supernova 2002ap in M74 IAU Circular 2002 7810 http://adsabs.harvard.edu/abs/2002IAUC.7810....1N and w:SN 2003gd.R. Evans, R. H. McNaught Supernova 2003gd in M74 IAU Circular 2003 8150 http://adsabs.harvard.edu/abs/2003IAUC.8150....2E SN 2002ap has attracted considerable attention because it is one of the few Type Ic supernovae (or w:hypernovae) observed within 10 Mpc in recent years.P. A. Mazzali, J. Deng, K. Maeda, K. Nomoto, H. Umeda, K. hatano, K. Iwamoto, Y. Yoshii, Y. Kobayashi, T. Minezaki, M. Doi, K. Enya, H. Tomita, S. J. Smartt, K. Kinugasa, H. Kawakita, K. Ayani, T. Kawabata, H. Yamaoka, Y. L. Qiu, K. Motohara, C. L. Gerardy, R. Fesen, K. S. Kawabata, M. Iye, N. Kashikawa, G. Kosugi, Y. Ohyama, M. Takada-Hidai, G. Zhao, R. Chornock, A. V. Filippenko, S. Benetti, M. Turatto The Type Ic Hypernova SN 2002ap Astrophysical Journal 2002 572 L61–L65 http://adsabs.harvard.edu/abs/2002ApJ...572L..61M 10.1086/341504S. J. Smartt, P. M. Vreeswijk, E. Ramirez-Ruiz, G. F. Gilmore, W. P. S. Meikle, A. M. N. Ferguson, J. H. Knapen On the Progenitor of the Type Ic Supernova 2002ap Astrophysical Journal 2002 572 L147–L151 http://adsabs.harvard.edu/abs/2002ApJ...572L.147S 10.1086/341747A. Gal-Yam, E. O. Ofek, O. Shemmer Supernova 2002ap: the first month Monthly Notices of the Royal Astronomical Society 2002 332 L73–L77 http://adsabs.harvard.edu/abs/2002MNRAS.332L..73G 10.1046/j.1365-8711.2002.05535.x This supernovae has been used to test theories on the origins of similar Type Ic supernovae at higher distances and theories on the connection between supernovae and w:gamma ray bursts. SN 2003gd is a Type II-P supernova.S. D. Van Dyk, W. Li, A. V. Filippenko On the Progenitor of the Type II-Plateau Supernova 2003gd in M74 Publications of the Astronomical Society of the Pacific 2003 115 1289–1295 http://adsabs.harvard.edu/abs/2003PASP..115.1289V 10.1086/378308 Type II supernovae have known luminosities, so they can be used to accurately measure distances. The distance measured to M74 using SN 2003gd is 9.6 ± 2.8 Mpc, or 31 ± 9 million ly.M. A. Hendry, S. J. Smartt, J. R. Maund, A. Pastorello, L. Zampieri, S. Benetti, M. Turatto, E. Cappellaro, W. P. S. Meikle, R. Kotak, M. J. Irwin, P. G. Jonker, L. Vermaas, R. F. Peletier, H. van Woerden, K. M. Exter, D. L. Pollacco, S. Leon, S. Verley, C. R. Benn, G. Pignata A study of the Type II-P supernova 2003gd in M74 Monthly Notices of the Royal Astronomical Society 2005 359 906–926 http://adsabs.harvard.edu/abs/2005MNRAS.359..906H 10.1111/j.1365-2966.2005.08928.x For comparison, distances measured using the brightest supergiants are 7.7 ± 1.7 Mpc and 9.6 ± 2.2 Mpc. Ben E. K. Sugerman found a "light echo" - a reflection of supernova explosion that appeared after the explosion itself - associated with SN 2003gd.B. E. K. Sugerman Discovery of a Light Echo from SN 2003gd Astrophysical Journal 2005 632 L17–L20 http://adsabs.harvard.edu/abs/2005ApJ...632L..17S 10.1086/497578 This is one of the few supernovae in which such a reflection has been found. This reflection appears to be from dust in a sheet-like cloud that lies in front of the supernova, and it can be used to determine the composition of the interstellar dust.S. D. Van Dyk, W. Li, A. V. Filippenko The Light Echo around Supernova 2003gd in Messier 74 Publications of the Astronomical Society of the Pacific 2006 118 351–357 http://adsabs.harvard.edu/abs/2006PASP..118..351V 10.1086/500225 Galaxy group information M74 is the brightest member of the w:M74 Group, a group of 5-7 galaxies that also includes the peculiar w:spiral galaxy w:NGC 660 and a few w:irregular galaxies.R. B. Tully 1988 Nearby Galaxies Catalog Cambridge University Press Cambridge 0-521-35299-1A. Garcia General study of group membership. II - Determination of nearby groups Astronomy and Astrophysics Supplement 1993 100 47–90 http://adsabs.harvard.edu/abs/1993A&AS..100...47GG. Giuricin, C. Marinoni, L. Ceriani, A. Pisani Nearby Optical Galaxies: Selection of the Sample and Identification of Groups Astrophysical Journal 2000 543 178–194 http://adsabs.harvard.edu/abs/2000ApJ...543..178G 10.1086/317070 Although different group identification methods may consistently identify many of the same member galaxies in this group, the exact group membership is still uncertain. Star formation thumb|250px|M74 as observed with the w:Spitzer Space Telescope as part of the w:Spitzer Infrared Nearby Galaxy Survey. The blue colors represent the 3.6 micrometre emission from stars. The green and red colors represent the 5.8 and 8.0 micrometre emission from w:polycyclic aromatic hydrocarbons and possibly dust. Suspected black hole In w:March 22, w:2005, it was announced Chandra :: Photo Album :: M74 :: 22 Mar 05 that the w:Chandra X-ray Observatory had observed an w:ultraluminous X-ray source (ULX) in M74, radiating more X-ray power than a w:neutron star in periodic intervals of around two hours. It has an estimated mass of around 10,000 w:Suns. This is an indicator of an w:intermediate-mass black hole. This would be a rather uncommon class of black holes, somewhere in between in size of stellar black holes and the massive black holes theorized to reside in the center of many galaxies. Because of this, they are believed to form not from single supernovae, but possibly from a number of lesser stellar black holes in a star cluster. The X-ray source is identified as CXOU J013651.1+154547. Amateur astronomy observation information Messier 74 is located 1.5° east-northeast of w:Eta Piscium. As stated above, the galaxy has the lowest surface brightness of all the Messier objects. It may be very difficult to see unless the sky is dark and clear, and it may be difficult to see in locations affected by w:light pollution. The galaxy may be best viewed under low magnification; when highly magnified, the diffuse emission becomes more extended and appears too faint to be seen by many people. Additionally, the galaxy may be more easily seen when using w:averted vision when the eyes are fully dark adapted. Messier 74 External links Spiral Galaxy M74 @ SEDS Messier pages References