Abstract
We report the result from observations conducted with the Atacama Large
Millimeter/submillimeter Array (ALMA) to detect CII 158 um fine structure
line emission from galaxies embedded in one of the most spectacular Lyman-alpha
blobs (LABs) at z=3.1, SSA22-LAB1. Of three dusty star-forming galaxies
previously discovered by ALMA 860 um dust continuum survey toward SSA22-LAB1,
we detected the CII line from one, LAB1-ALMA3 at z=3.0993+/-0.0004. No line
emission was detected, associated with the other ALMA continuum sources or from
three rest-frame UV/optical selected z_spec~3.1 galaxies within the field of
view. For LAB1-ALMA3, we find relatively bright CII emission compared to the
infrared luminosity (L_CII/L_CII) and an extremely high CII 158 um and
NII 205 um emission line ratio (L_CII/L_NII>55). The relatively strong
CII emission may be caused by abundant photodissociation regions and
sub-solar metallicity, or by shock heating. The origin of the unusually strong
CII emission could be causally related to the location within the giant LAB,
although the relationship between extended Lyman-alpha emission and ISM
conditions of associated galaxies is yet to be understand.
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