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Table 2:

Properties of the host galaxies of ULXs in C-COSMOS.

XIDa 		i mag $R_{\rm P}$b zc Classd log($M_\star$) SFR
  (AB) (arcsec)     ($M_\odot$) ($M_\odot$/yr)
1151e 15.62 19.89 $0.094 ^{\rm p}$ ETG ... ...
1388 20.39 5.20 0.204 $^{\rm p}$ LTG $\rm 10.1^{+0.2}_{-0.1}$ $\rm 3.0^{+0.8}_{-1.1}$
1870 18.40 9.21 0.072 $^{\rm s}$ LTG $\rm 9.9^{+0.2}_{-0.1}$ $\rm 1.3^{+0.4}_{-0.2}$
2418 19.45 3.99 0.283 $^{\rm s}$ ETG $\rm 10.9^{+0.1}_{-0.1}$ $\rm0.3^{+0.1}_{-0.1}$
3441 18.19 5.50 0.133 $^{\rm s}$ LTG $\rm 10.5^{+0.1}_{-0.3}$ $\rm 1.1^{+0.1}_{-0.1}$
11100 18.48 6.90 0.110 $^{\rm s}$ LTG $\rm 10.4^{+0.1}_{-0.1}$ $\rm 1.7^{+0.1}_{-0.1}$
11938 18.94 2.53 0.221 $^{\rm p}$ ETG $\rm 10.9^{+0.1}_{-0.1}$ $\rm0.04^{+0.12}_{0.01}$

Notes. (a) ID of the Chandra source (Elvis et al. 2009). (b) Petrosian radius of the host galaxy Petrosian (1976). (c) Redshift of the host galaxy: ``s'' for spectroscopic and ``p'' for photometric redshifts. (d) Morphologi- cal classification of the ULX host galaxy: early type galaxy (ETG) or late type galaxy (LTG). (e) The photometric coverage is limited to few bands and we cannot constrain its $M_\star$ or SFR.


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