The atmospheres of planetary objects contain natural dust particles, and planetary scientists call them aerosols or haze particles. The chemical and physical properties of the haze particles in the atmospheres of Jupiter, Saturn, and Titan have been revealed by Cassini and Juno: the Saturn and Jupiter space missions, respectively. Cassini arrived at the Saturnian system in 2006, and Juno at the Jovian system in 2016. We analyzed infrared spectra from these missions in order to extract haze spectra from raw spectra, which are heavily entangled by molecular lines, especially by strong CH4 emission and absorption lines. We first analyzed the 3.0-3.5 and 2.0-2.5 mm spectra of Titan observed by Cassini/VIMS, a near-IR camera and spectrometer. Surprisingly, we found that the haze spectra of Titan are very different from the typical spectra of ‘tholins’, which have been laboratory-made and claimed by Carl Sagan for the haze particles in the atmospheres of Titan, Saturn, and Jupiter for more than 40 years. The derived haze spectra of Titan are, instead, very similar to the typical spectra of aromatic hydrocarbons at high altitudes and aliphatic hydrocarbons at low altitudes. The tholins were even considered to be one of the important components of interstellar dust particles. We also analyzed the Cassini/VIMS 3.0-3.5 mm spectra of Saturn to extract Saturnian haze spectra. We found that the polar haze is dominated by aromatic hydrocarbons while the haze at lower latitudes mostly consists of aliphatic hydrocarbons. This spectral variation in the di?erent latitudinal regions suggests that newly created haze particles at the high altitudes in the auroral regions of Saturn undergo an aging process mainly during latitudinal advection/di?usion from the polar atmosphere to the low altitude and low latitudinal regions, while in the atmosphere of Titan, the aging process mainly occurs during the vertical precipitation process of haze. Recently, we analyzed the 2.0-2.5 mm spectra of Jupiter’s polar regions observed by Juno/JIRAM, another camera and spectrometer very similar to Cassini/VIMS. We were able to extract the haze spectra of the polar regions of Jupiter; and found that the spectra are roughly similar to those of Titan suggesting similar chemical and physical processes of haze particles in the atmosphere of Jupiter.