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We conduct a systematic search for galaxies at $z=0.1-1.5$ with[OII]$\lambda3727$, [OIII]$\lambda5007$, or H$\alpha\lambda6563$ emission linesextended over at least 30 kpc by using deep narrowband and broadband imaging inSubaru-XMM Deep Survey (SXDS) field. These extended emission-line galaxies aredubbed [OII], [OIII], or H$\alpha$ blobs. Based on a new selection method thatsecurely selects extended emission-line galaxies, we find 77 blobs at$z=0.40-1.46$ with the isophotal area of emission lines down to$1.2\times10^{-18}$ erg s$^{-1}$ cm$^{-2}$ kpc$^{-2}$. Four of them arespectroscopically confirmed to be [OIII] blobs at $z=0.83$. We identify AGNactivities in 8 blobs with X-ray and radio data and find that the fraction ofAGN contribution increases with increasing isophotal area of the extendedemission. With the Kolmogorov-Smirnov (KS) and Anderson-Darling tests, weconfirm that the stellar-mass distributions of H$\alpha$ and [OII] blobs arenot drawn from those of the emitters at the $>90$% confidence level in thatH$\alpha$ and [OII] blobs are located at the massive end of the distributions,but cannot reject null hypothesis of being the same distributions in terms ofthe specific star formation rates. It is suggested that galactic-scale outflowstend to be more prominent in more massive star-forming galaxies. Exploiting oursample homogeneously selected over the large area, we derive the numberdensities of blobs at each epoch. The number densities of blobs decreasedrastically with redshifts at the rate that is larger than that of the decreaseof cosmic star formation densities.

Systematic Survey for [OII], [OIII], and H$\alpha$ Blobs at $z=0.1-1.5$: The Implication for Evolution of Galactic-Scale Outflow