The galaxy Messier 101 is a swirling spiral of stars, gas, and dust. Messier 101 is nearly twice as wide as our Milky Way Galaxy.
Spitzer's view [left frame], taken in infrared light, reveals the galaxy's delicate dust lanes as yellow-green filaments. Such dense dust clouds are where new stars can form. In this image, dust warmed by the light of hot, young stars glows red. The rest of the galaxy's hundreds of billions of stars are less prominent and form a blue haze. Astronomers can use infrared light to examine the dust clouds where stars are born.
Messier 101 has a pancake-like shape that we view face-on. This perspective shows off the spiral structure that gives it the nickname the Pinwheel Galaxy. In this Hubble image [middle frame], taken in visible light, the bright blue clumps are regions where new stars have formed. The yellowish core consists mainly of old stars. The dark brown dust lanes are colder and denser regions where interstellar clouds may collapse to form new stars. All of these features are shaped into a beautiful spiral pattern by a combination of gravity and rotation. Astronomers use visible light to study where and how stars form in spiral galaxies.
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.
The International Year of Astronomy Great Observatories Image Unveiling is supported by the NASA Science Mission Directorate Astrophysics Division. The project is a collaboration between the Space Telescope Science Institute, the Spitzer Science Center, and the Chandra X-ray Center.
Credits
Spitzer Image: NASA, Jet Propulsion Lab/Caltech, and K. Gordon (STScI);Hubble Image: NASA, ESA, K. Kuntz (JHU), F. Bresolin (University of Hawaii), J. Trauger (Jet Propulsion Lab), J. Mould (NOAO), Y.-H. Chu (University of Illinois, Urbana), and STScI;
Chandra Image: NASA, CXC, and K. Kuntz (JHU)
| About The Object | |
|---|---|
| Object Name | M101, NGC 4547, The Pinwheel Galaxy |
| Object Description | Face-on Spiral Galaxy |
| R.A. Position | 14h 3m 13.0s |
| Dec. Position | 54° 20' 52.99" |
| Constellation | Ursa Major |
| Distance | 21.8 million light-years (6.7 megaparsecs) |
| Dimensions | This image is 18 arcminutes (114,000 light-years or 35,000 parsecs) wide. |
| About The Data | |
| Data Description | Spitzer data (left): The science team for the Spitzer data include K. Gordon (STScI), C. Engelbracht, G. Rieke, K. Misselt, and J.-D. Smith (University of Arizona), and R. Kennicutt (University of Cambridge). Hubble data (center): This image was created from HST data from the following proposals: : K. Kuntz (Johns Hopkins University) : F. Bresolin (University of Hawaii) : J. Trauger (Jet Propulsion Laboratory) : J. Mould (NOAO) : Y.-C. Chu (University of Illinois, Urbana) The Hubble exposures have been superimposed onto ground-based images, visible at the edge of the image, taken at the Canada-France-Hawaii Telescope in Hawaii, and at the 0.9-meter telescope at Kitt Peak National Observatory, part of the National Optical Astronomy Observatory in Arizona. Chandra data (right): The science team was led by K. Kuntz (Johns Hopkins University). |
| Instrument | Spitzer>IRAC, Spitzer>MIPS, HST>ACS/WFC, HST>WFPC2, and CXO>ACIS |
| Exposure Dates | Mar 8, 2004 and May 10/11, 2004 (Spitzer), March 1994, September 1994, June 1999, November 2002, and January 2003 (HST), and March 2000 - January 2005 (CXO) |
| Filters | Spitzer: 85 sec/pixel (IRAC) and 200 sec/pixel (MIPS 24 micron) HST: F435W (B), F555W (V)), and F814W (I) CXO Energies: 0.45 - 1.00 keV and 1.00 - 2.00 keV |
| About The Object | |
|---|---|
| Object Name | A name or catalog number that astronomers use to identify an astronomical object. |
| Object Description | The type of astronomical object. |
| R.A. Position | Right ascension – analogous to longitude – is one component of an object's position. |
| Dec. Position | Declination – analogous to latitude – is one component of an object's position. |
| Constellation | One of 88 recognized regions of the celestial sphere in which the object appears. |
| Distance | The physical distance from Earth to the astronomical object. Distances within our solar system are usually measured in Astronomical Units (AU). Distances between stars are usually measured in light-years. Interstellar distances can also be measured in parsecs. |
| Dimensions | The physical size of the object or the apparent angle it subtends on the sky. |
| About The Data | |
| Data Description |
|
| Instrument | The science instrument used to produce the data. |
| Exposure Dates | The date(s) that the telescope made its observations and the total exposure time. |
| Filters | The camera filters that were used in the science observations. |
| About The Image | |
| Image Credit | The primary individuals and institutions responsible for the content. |
| Publication Date | The date and time the release content became public. |
| Color Info | A brief description of the methods used to convert telescope data into the color image being presented. |
| Orientation | The rotation of the image on the sky with respect to the north pole of the celestial sphere. |
