Systematic Survey for [OII], [OIII], and H$\alpha$ Blobs at $z=0.1-1.5$:
  The Implication for Evolution of Galactic-Scale Outflow
  We conduct a systematic search for galaxies at $z=0.1-1.5$ with
[OII]$\lambda3727$, [OIII]$\lambda5007$, or H$\alpha\lambda6563$ emission lines
extended over at least 30 kpc by using deep narrowband and broadband imaging in
Subaru-XMM Deep Survey (SXDS) field. These extended emission-line galaxies are
dubbed [OII], [OIII], or H$\alpha$ blobs. Based on a new selection method that
securely 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 are
spectroscopically confirmed to be [OIII] blobs at $z=0.83$. We identify AGN
activities in 8 blobs with X-ray and radio data and find that the fraction of
AGN contribution increases with increasing isophotal area of the extended
emission. With the Kolmogorov-Smirnov (KS) and Anderson-Darling tests, we
confirm that the stellar-mass distributions of H$\alpha$ and [OII] blobs are
not drawn from those of the emitters at the $>90$% confidence level in that
H$\alpha$ and [OII] blobs are located at the massive end of the distributions,
but cannot reject null hypothesis of being the same distributions in terms of
the specific star formation rates. It is suggested that galactic-scale outflows
tend to be more prominent in more massive star-forming galaxies. Exploiting our
sample homogeneously selected over the large area, we derive the number
densities of blobs at each epoch. The number densities of blobs decrease
drastically with redshifts at the rate that is larger than that of the decrease
of cosmic star formation densities.
