The primary objective of SM1 was to replace the telescope's solar arrays, which had degraded over time and were no longer providing enough power to operate the telescope.

There were a total of 5 Hubble Space Telescope Servicing Missions (SM1-SM5) conducted between 1993 and 2009.

The WFPC2 instrument was installed during SM1 in 1993. It was a significant upgrade to the telescope's capabilities, allowing for wider field of view and improved sensitivity.

The STIS instrument was designed to study the composition of stars and galaxies by analyzing the light they emit across a wide range of wavelengths.

SM3, conducted in 1999, included the repair of the telescope's primary mirror, which had a manufacturing defect that caused spherical aberration.

The ACS instrument was designed to survey large areas of the sky in multiple wavelengths, enabling astronomers to study the distribution and evolution of galaxies, stars, and other celestial objects.

The COS instrument was installed during SM4 in 2009. It is a spectrograph designed to study the chemical composition and physical properties of stars, galaxies, and other astronomical objects.

The WFC3 instrument was designed to take high-resolution images of galaxies, nebulae, and other celestial objects in both visible and infrared light.

SM5, conducted in 2009, was the final servicing mission for the Hubble Space Telescope. It included repairs to the telescope's instruments and systems, as well as the installation of new batteries and gyroscopes.

The main goal of the Hubble Space Telescope's servicing missions was to extend the telescope's lifespan, upgrade its scientific capabilities, and repair and maintain its instruments and systems.

The NICMOS instrument was installed during SM2 in 1997. It was designed to observe objects in the near-infrared spectrum, allowing astronomers to study cool objects like stars and planets.

The STIS instrument was designed to study the composition of stars and galaxies by analyzing the light they emit across a wide range of wavelengths.

SM3, conducted in 1999, included the repair of the telescope's primary mirror, which had a manufacturing defect that caused spherical aberration.

The ACS instrument was designed to survey large areas of the sky in multiple wavelengths, enabling astronomers to study the distribution and evolution of galaxies, stars, and other celestial objects.

The COS instrument was installed during SM4 in 2009. It is a spectrograph designed to study the chemical composition and physical properties of stars, galaxies, and other astronomical objects.