Messier 101 (M101), also known as the Pinwheel Galaxy, is a spiral galaxy located in the constellation Ursa Major, the Great Bear. The Pinwheel Galaxy has an apparent magnitude of 7.86 and lies at a distance of 20.9 million light years from Earth. It has the designation NGC 5457 in the New General Catalogue.
The galaxy appears face-on and occupies an area of 28.8 by 26.9 arc minutes of apparent sky, which corresponds to a linear diameter of about 170,000 light years. The galaxy is quite large, but has a low surface brightness and requires exceptionally clear, moonless skies to be seen, even in medium-sized telescopes.
The Pinwheel Galaxy can be spotted in 10×50 binoculars under exceptionally good conditions, but only appears as a large, faint patch of light. Small telescopes only reveal the galaxy’s brighter central region, while the spiral structure appears as patchy nebulosity in 4-inch instruments. 8-inch telescopes show the galaxy’s dense core surrounded by a fainter halo dotted with patches of nebulosity and hinting at the spiral structure.
Messier 101 is easy to find because it is located just above the handle of the Big Dipper. It forms a triangle with Alkaid and the double star Mizar/Alcor. It can be found 5.5 degrees northeast of Alkaid and at the same angular separation from Mizar. The best time of year to observe the Pinwheel Galaxy is during the spring.
Messier 101 is estimated to contain 1 trillion stars. Young and old stars appear to be evenly distributed along the galaxy’s spiral arms, as revealed by combined images of M101 in visible, infrared and X-ray wavelengths.
The galaxy has an unusually high number of H II regions, where new stars form, and many of these regions are bright and large, ionized by many extremely luminous and hot young stars. Observations in 1991 led to the discovery of 1,264 H II regions in M101. Three of these were bright enough to get their own designations in the New General Catalogue: NGC 5461, NGC 5462 and NGC 5471.
With a linear extension of 170,000 light years, the Pinwheel Galaxy is about 70 percent larger than the Milky Way. The estimated mass of M101’s disk is about 100 billion solar masses, while its small central bulge has a mass 3 billion times that of the Sun. The galaxy has an absolute magnitude of -21.6, corresponding to a luminosity of 30 billion Suns.
Such composite images allow astronomers to see how features seen in one wavelength match up with those seen in another wavelength. It’s like seeing with a camera, night vision goggles, and X-ray vision all at once. Image: NASA, ESA, CXC, JPL, Caltech and STScI
The galaxy does not appear to have a supermassive black hole at its centre, as observations in radio and X-ray wavelengths have not detected a strong source of emissions in the galactic core.
The Pinwheel Galaxy appears symmetric in images that only reveal its central region, but is really quite asymmetrical as a result of interactions with smaller companion galaxies. The galaxy’s core is displaced from the centre, likely as a result of a collision in the recent past.
M101 has five prominent companions: NGC 5204, NGC 5474, NGC 5477, NGC 5585 and Holmberg IV. Gravitational interaction with these galaxies is suspected to have triggered the formation of the grand design structure in M101 and distorted NGC 5474.
Chandra’s image of Messier 101 [right frame], taken in X-ray light, shows the high-energy features of this spiral galaxy. X-rays are generally created in violent and/or high-temperature events. The white dots are X-ray sources that include the remains of exploded stars as well as material colliding at extreme speeds around black holes. The pink and blue colors are emission from million-degree gas and from clusters of massive stars. The pink emission indicates lower-energy X-rays and the blue higher-energy X-rays. One reason astronomers study Messier 101’s X-rays is to better understand how black holes grow in spiral galaxies. Image: NASA, ESA, CXC, JPL, Caltech and STScI
An image of M101 taken by the Hubble Space Telescope in 2006 was the largest and most detailed image of a galaxy to date, composed from 51 individual exposures and several ground-based images.
Three supernovae were discovered in M101 in the 20th century: SN 1909A (peculiar type, mag. +12.1) in January 1909 SN 1951H (Type II, mag. +17.5) in September 1951, and SN 1970G (Type II, mag. +11.5) in January 1970.
Another supernova was detected in the Pinwheel Galaxy by the Palomar Transient Factory (PTF) on August 24, 2011 at magnitude 17.2. Designated as SN 2011fe, it was classified as a Type Ia supernova, one triggered by a violent explosion of a white dwarf. It brightened to magnitude 9.9 around September 10 and was the nearest supernova seen since 1987.
This image is part of a “quartet of galaxies” collaboration of professional and amateur astronomers that combines optical data from amateur telescopes with data from the archives of NASA missions. NASA’s Marshall Space Flight Center in Huntsville, Ala., manages the Chandra program for NASA’s Science Mission Directorate in Washington. The Smithsonian Astrophysical Observatory in Cambridge, Mass., controls Chandra’s science and flight operations. Image – X-ray: NASA/CXC/SAO; Optical: Detlef Hartmann; Infrared: NASA/JPL-Caltech
Observations with the Chandra X-ray Observatory identified the X-ray source P98 as an ultra-luminous X-ray source in 2001. An ultra-luminous X-ray source is a source of X-ray emissions more powerful than a single star, but not as powerful as an entire galaxy. The source was designated as M101 ULX-1. Observations with the Hubble Space Telescope and ESA’s orbiting X-ray observatory XMM-Newton revealed that the source had an optical counterpart, indicating that it was an X-ray binary system.
Messier 101 was discovered by the French astronomer Pierre Méchain on March 27, 1781. Méchain reported the discovery to his colleague Charles Messier, who verified the object’s position and added it to his catalogue with the following note:
Nebula without star, very obscure & pretty large, of 6 or 7 minutes [of arc] in diameter, between the left hand of Boötes & the tail of the great Bear. It is difficult to distinguish when one lits the [grating] wires. (diam. 7′)
William Herschel observed M101 with his 20-foot telescope on September 20, 1783 and wrote:
In the northern part is a large star pretty distinctly seen, and in the southern I saw 5 or 6 small ones glitter through the greatest nebulosity which appears to consist of stars. Evening bad. This and the 51st [Whirlpool Galaxy, M51] are both so far removed from the appearance of stars that it is the next step to not being able to resolve them. My new 20 feet will probably render it easy.
Herschel catalogued several of M101’s spiral arm fragments on April 14, 1789, three of which were later assigned their own NGC numbers: H III.787 (NGC 5447), H III.788 (NGC 5461) and H III. 789 (NGC 5462). Herschel wrote:
Very bright, small nucleus with extensive nebulosity, pretty well determined on the preceding [W] side, but very diffuse to the north following [NE]. Includes the two following nebulae [III.788 and 789, NGCs 5461, 5462], and seems to extend 20′, perhaps 30′ or more.
John Herschel catalogued M101 as h 1744 and later added it to his General Catalogue as GC 3770. He described the object as “pretty bright; very large; irregularly round; gradually, then very suddenly, much brighter toward the middle, where there is a bright small nucleus.”
Admiral William Henry Smyth observed M101 in April 1837 and offered more details:
A pale white nebula, in the nebulous field np the right hand of Boötes; it is 5d north-north-east of Alkaid, and a similar distance east-half-south from Mizar. This object was discovered by Méchain in 1781, in whose instruments it was very obscure; and it only exhibited a mottled nebulosity to WH [William Herschel]. Under a very favourable view it is large and well spread, though somewhat faint except towards the centre, where it brightens. There are several telescopic stars in the field, one of which is very close to the nebula.
From the nature of this neighbourhood, and a trifling uncertainty in the earlier data, this object may be 214 H I [this is actually NGC 5474]; but that astronomer does not appear to have been aware of the identity. It is one of those globular nebulae that seem to be caused by a vast agglomeration of stars, rather than by a mass of diffused luminous matter; and though the idea of too dense a crowd may intrude, yet the paleness tells of its inconceivable distance, and probable discreteness.
William Parsons, 3rd Earl of Rosse observed the object in his 72-inch Newtonian reflector on eight different occasions and sketched it. He was the first to note the spiral structure in M101. He wrote, “Sketched 3 times. Mar. 1, 1851. Large spiral; faintish; several arms and knots; 14′ across at least.”
Heber Curtis photographed the object with the 36-inch Crossley reflector at the Lick Observatory and wrote:
This unusually beautiful spiral is about 16′ in diameter. There is an almost stellar nucleus, with two bright condensations very close which give a tri-nuclear appearance. The open whorls show a multitude of stellar condensations. [NGCs] 5449, 5450, 5451, 5453, 5455, 5458, 5461, 5462, are simply brighter knots in the great nebula. 10 s.n.
Halton Arp included M101 as Arp 26 in his Atlas of Peculiar Galaxies as a “Spiral with One Heavy Arm”.
FACTS
| Object: Galaxy |
| Type: Spiral |
| Class: SAB(rs)cd |
| Designations: Messier 101, M101, NGC 5457, Pinwheel Galaxy, Arp 26, PGC 50063, UGC 8981, APG 26, K73 610, IRAS 14013+5435, 2MASX J14031258+5420555, MCG+09-23-028, SDSS J140312.52+542056.2, SPB 243, TC 302, VV 344, VV 344a, VV 456, UZC J140312.5+542056, Z 272-21, Z 1401.5+5435 |
| Constellation: Ursa Major |
| Right ascension: 14h 03m 12.6s |
| Declination: +54°20’57” |
| Distance: 20.9 million light years (6.4 megaparsecs) |
| Number of stars: 1 trillion |
| Apparent magnitude: +7.86 |
| Absolute magnitude: -21.6 |
| Apparent dimensions: 28′.8 x 26′.9 |
| Radius: 85,000 light years |
| Redshift: 0.000804 |
| Helio radial velocity: 241 km/s |
LOCATION
