the carme group is a group of retrograde irregular satellites of jupiter that follow similar orbits to carme and are thought to have a common origin. their semi-major axes (distances from jupiter) range between 22.9 and 24.1 gm, their orbital inclinations between 164.9Â° and 165.5Â°, and their orbital eccentricities between 0.23 and 0.27 (with one exception).  the core members include (from largest to smallest): scott s. sheppard, david c. jewitt, carolyn porco jupiter's outer satellites and trojans, in: jupiter. the planet, satellites and magnetosphere. edited by fran bagenal, timothy e. dowling, william b. mckinnon. cambridge planetary science, vol. 1, cambridge, uk: cambridge university press, isbn 0-521-81808-7, 2004, p. 263 - 280 full text(pdf). david nesvornÃ½, cristian beaugÃ©, and luke dones collisional origin of families of irregular satellites, the astronomical journal, 127 (2004), pp. 1768â1783 full text. thumb|right|300px|this diagram compares the orbital elements and relative sizes of the core members of the carme group. the horizontal axis illustrates their average distance from jupiter, the vertical axis their orbital inclination, and the circles their relative sizes. * carme (the largest, which gives its name to the group) * taygete * eukeladelisted by nesvorny 2004 as a possible member, not listed by sheppard 2004; the orbital elements confirmed by jacobson 2004 * s/2003 j 5 * chaldene * isonoe * kalyke (substantially redder than the others) * erinome * aitne * kale * pasithee * s/2003 j 9 * s/2003 j 10 the international astronomical union (iau) reserves names ending in -e for all retrograde moons, including this group's members. ==origin== the very low dispersion of the mean1 orbital elements among the core members (the group is separated by less than 700,000&nbsp;km in semi major axis and less than 0.7Â° in inclination) suggests
Carme_group Irregular_satellites Moons_of_Jupiter