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Text: The sample is described in detail in Conselice et al . ( 2007 ) and Trujillo et al . ( 2007 ) . Briefly , the K - band survey covers 2165 arcmin 2 in the EGS and has a depth K=22.5 mag ( 5σ ) . Only 710 arcmin 2 are covered simultaneously with HST / ACS v - and i - band imaging from the All - Wavelength Extended Groth Strip International Survey ( AEGIS , Davis et al . 2007 ) , so reliable structural parameters can only be measured for 831 galaxies within the entire POWIR / DEEP-2 survey in EGS . Half of those 831 galaxies has spectroscopic redshifts based on optical data obtained by the DEEP-2 Galaxy Redshift survey ( Davis et al . 2003 ) . Conselice et al . ( 2007 ) estimate photometric redshifts for the rest of sources with an accuracy ∆z/(1 + z)=0.025 . The 831 galaxies with M>10 11 M ⊙ in the EGS lie in the red - shift range 0.2 < z 2 . Stellar masses were estimated by Bundy et al . ( 2005Bundy et al . ( , 2006 using the exponential star formation models of Bruzual & Charlot ( 2003 ) with a Chabrier ( 2003 ) IMF and various ages , metallicities and dust contents included . As shown by Conselice et al . ( 2007 ) , typical uncertainties in the stellar masses are a factor of ∼2 ( typical of any stellar population study ; see , e.g. , Pérez - González et al . 2003 , Kauffmann et al . 2003 , Papovich et al . 2006 , Fontana et al . 2006 . As discussed in detail in Conselice et al . ( 2007 ) , this factor includes the effects of the photometric redshift uncertainties , the errors inherent to solution degeneracies , and the choices of the IMF and the stellar emission library . For example , using Maraston ( 2005 ) models ( with an improved treatment of the TP - AGB stellar evolution phase ) would produce a 20 % ( at most ) systematic decrease in the mass estimations . Using a Salpeter ( 1955 ) IMF would increase the stellar masses by a constant factor of 0.25dex . Trujillo et al . ( 2007 ) estimated ( circularized ) half - light radius ( r e ) and Sérsic ( 1968 ) indices ( n ) for all the galaxies in our sample . They used i - band HST / ACS images to fit surface brightness profiles and divided the sample in disk - like and spheroid - like galaxies according to the value of the Sérsic index . Ravindranath et al . ( 2004 , see also Andredakis et al . 1995 demonstrated that nearby galaxies with n<2.5 are mostly disks , while spheroids are characterized by high Sérsic indices , n>2.5 . They also performed simulations to check that the Sérsic index obtained from HST data can be used as a morphology indicator at z>0 . Trujillo et al . ( 2007 ) extended these simulations to prove that the structural parameters are robust against the effects introduced by K - corrections , AGN contamination , and surface brightness dimming .<|eot_id|><|start_header_id|>assistant<|end_header_id|>

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