Fig 1. The spiral galaxy NGC 1309.
Fig 2. NGC 4145, an anemic spiral in the Ursa Major cluster of galaxies. While the spiral arms of this galaxy are punctuated by some activity, the rest of the galaxy is quite quiet. The likelihood is that a galaxy like this will soon (in galactic terms) lose the impetus to form stars and settle down to become a lenticular galaxy. Image credit : NOAO.
Fig 3. The barred spiral NGC 4725. Image courtesy Richard Crisp.
A spiral galaxy is a galaxy with a flattened disk and a nuclear bulge from which emanate luminous spiral arms (Fig 1). As well as stars, the disk harbors extensive interstellar clouds of gas and dust. Surrounding the disk is a large galactic halo. There are two main types of spiral galaxy – barred spirals (type SB) and ordinary spirals (type S), each of which is divided into subtypes a (tightly wound arms, large bulge), b, c, and (sometimes) d (loosely wound arms, small bulge). The trend from a to d is toward decreasing brightness and mass. Spiral galaxies and lenticular galaxies together make up the class known as disk galaxies.
In diameter, spirals range from about 10,000 to over 300,000 light-years, and in mass from about one billion to 500 billion solar masses. Spiral structure can apparently exist only in disk galaxies above a certain size and, although spirals represent 80% of the bright galaxies in regions outside of rich clusters (those having many members within a relatively compact region of space), there are no spirals with masses as low as those of many irregular galaxies and dwarf ellipticals.
Our own Milky Way Galaxy, together with the nearby Andromeda Galaxy, are both large spiral galaxies. Other relatively close and well known spirals include the Triangulum Galaxy, the Whirlpool Galaxy, the Sunflower Galaxy, the Black Eye Galaxy, the Sombrero Galaxy, M74, M81, and M101.
|Fig 3. The spiral galaxy NGC 2997 with well-defined spiral arms.
A spiral arm is a curved feature, containing young stars, open clusters, HII regions, and dust, that winds outward from the nucleus of a spiral galaxy into the disk (Fig 3). Usually two arms are present that wrap around in a well-defined pattern; however, some spirals have four or, in rare cases, three arms, in an arrangement that may complex and fragmentary. The arms are visible because of bright, massive stars, the formation of which is triggered by the movement through the disk of a density wave.
The galactic bulge is the spheroidal mass of stars that forms the central hub of spiral and lenticular galaxies – the yoke, if such galaxies are imagined to resemble fried eggs. The bulge diminishes in size relative to the galactic disk in the sequence of spirals Sa to Sd. Stars that populate the bulge are normally old, Population II objects, dating back to their galaxy's earliest period. Studying bulges can therefore tell astronomers about how galaxies formed and evolved.
According to one current theory, a spiral galaxy begins as a giant, roughly spherical rotating mass of gas and dust, which gradually flattens out at the edges to create the disk. The original spherical shape lives on in the outermost region of a galaxy, known as the galactic halo, and, to a lesser extent, in the bulge. However, this view is challenged by observations of some bulges. The bulge of the Triangulum Galaxy (M33), for example, contains young- and intermediate-age stars, and has a star distribution that suggests the disk goes all the way to the center. This raises questions about how M33 as a whole formed and what triggered the birth of the relatively youthful stars in its bulge.
Anemic spiral galaxy
An anemic spiral galaxy is a galaxy with characteristics that are intermediate between those of a normal spiral galaxy and a lenticular galaxy (Fig 2). Anemic spirals have smooth, weak spiral arms and a reduced rate of star formation linked to their deficiency in neutral hydrogen gas. They tend to occur in rich clusters of galaxies, suggesting that they may have been stripped of interstellar material through multiple encounters with other galaxies. This raises the question of whether anemic spirals mark both a morphological and an evolutionary transition between normal spirals and lenticulars.
Barred spiral galaxy
A barred spiral galaxy (Fig 3) is a type of spiral galaxy with a rectangular or cigar-shaped nucleus, from the ends of which spiral arms extend. Bars are large bodies of gas, dust, and stars that rotate as if they were solid objects. Typically they are 2 to 5 times longer than they are wide and may contribute up to one-third of a galaxy's luminosity. By channeling gas and dust to the center of the galaxies, they may trigger bursts of star formation, or, alternatively, feed material to a supermassive black hole in the galactic core.
Bars are believed to represent a temporary stage in the life of some spiral systems. According to one theory, they form spontaneously through global disturbances in disk galaxies. Another theory suggests they come about from interactions with nearby galaxies.
Barred galaxies are grouped by their appearance using three criteria: the central bulge and light distribution; the tightness with which the spiral arms are wound; and the degree to which the spiral arms are resolved into stars and nebulae. The three main types are SBa, SBb, and SBc.
The Tully-Fisher relation is an observed relation between the luminosity of spiral galaxies and their maximum rotation velocity. The Tully-Fisher relation is used as a way of estimating distances to spirals. The form is a linear relation between the absolute magnitude of a galaxy and the logarithm of the velocity at the flat part of the rotation curve, although the slopes and intercepts of these relations are different for Sa, Sb, and Sc type galaxies. Approximations made in deriving the relation are that the mass-to-light ratios are constant for all galaxies and that the average surface brightness of all galaxies is also equal.