In: Wagner W., Székely, В. (eds.): ISPRS ТС VII Symposium - 100 Years ISPRS, Vienna, Austria, July 5-7, 2010, IAPRS, Vol. XXXVIII, Part 7B 
Figure 1. VNIR-SWIR (A) and TIR (B) spectral characteristics 
of common minerals exist in ultramafic rocks. 
The common rock units in ophiolite sequence can be mafic or 
ultramafic. When the electromagnetic energy interactions with 
those rock types were compared (figure 2), the absorptions in 
8.63, 10.16 and 11.05 for diabase, 9.21 and 10.25 for gabbro, 
and 8.86, 9.57, 10.33 and 11.81 micrometer wavelengths for 
olivine-peridotite (dunite) are noticeable. On the contrary, the 
distinct reflections in wavelengths are 8.56, 9.10, 9.80 and 11.15 
for diabase, 8.77, 10.07 and 10.47 for gabbro, and 9.52, 10.17, 
10.58 and 11.92 micrometers for olivine-peridotite rocks. 
Figure 2. The spectral responses of abundant mafic and 
ultramafic rock types exist in ophiolite. 
1.2 Study Area 
Study area is located within the latitudes of 40°20' - 40°45N 
and the longitudes of 33°10'- 33°35'E in the northern part of 
Central Anatolia (Figure 3). There have been conducted various 
studies covering the area concentrated mainly on regional and 
local geological features, tectonics and kinematics, 
paleogeographic evolution etc. (Flakyemez et al, 1986; Tiirkecan 
et al, 1991, Koqyigit et al, 1995; Seyitoglu et al, 1997; Sumer, 
1997; Gokalp, 1999, Kaymakqi et al, 2003a, b). 
Figure 3. Location and simplified geological map of study area. 
The green (dark) colour in geological map represents 
ophiolitic lithologies. 
Study area is located at izmir-Ankara-Erzincan suture zone 
occurred as a northern branch of Neo-Tethys Ocean and started 
to activate in Liassic-Late Cretaceous and continued up to Early 
Lutetian presented by many authors (Akylirek et al, 1979, 1980, 
1981; §engor and Yilmaz, 1981; Górür et al, 1984; Hakyemez et 
al, 1986). Settlement time of ophiolite, which is a cause of 
closure of micro-continents (§engor and Yilmaz, 1981; Górür et 
al, 1984; Hakyemez et al, 1986; Kaymakqi et al, 2003a, b), is 
recorded as Cenomanian-Turonian age (Akyürek et al, 1979, 
1980, 1981). Tertiary shallow platform sedimentary sequence 
existed (Sengor and Yilmaz, 1981; Górür et al, 1984; Hakyemez 
et al, 1986; Seyitoglu et al, 1997) after Middle Lutetian 
subsequent to closure of Neo-Tetis Ocean in Early Lutetian 
(Hakyemez et al, 1986). The geological units and stratigraphy 
are simplified concerning to the objective lithologies of this 
study (Figure 3 and Figure 4). 
2. IMAGE ANALYSES, RESULTS AND DISCUSSION 
Well known ASTER (Advanced Spaceborne Thermal Emission 
and Reflection Radiometer) level 3A01 ortho image data which 
was corrected to remove the geographic distortion caused by 
altitudes is used in order to identify olivine-rich ultramafic rocks. 
ASTER has spatial resolution of 15 meter for 3 VNIR (Visible- 
near infrared, 0.556 to 0.807 micrometers) bands, 30 meter for 6 
SWIR (Short-wave infrared, 1.656 to 2.400 micrometers) bands 
and 90 meter for 5 TIR (Thermal infrared, 8.291 to 11.318 
micrometers) bands, and radiometric resolution of 8 bit, and 12 
bit for VNIR-SWIR and TIR respectively. 
AST3A10207260852290603310610, AST3A10507270844 
010603311228 and AST3A10404100850300702020025 images 
were used in the image analyses. The study area was cut after 
mosaicking those three images. During VNIR-SWIR band ratio 
image preparation, the masked image was used for better results. 
Results obtained from VNIR, SWIR and TIR are frequently 
efficient to extract information regarding to alteration mineral or 
lithological mapping from target area (Ninomiya, 2002; 
Yamaguchi and Naito, 2003; San et al., 2004; Rowan et al.,