TY - JOUR
T1 - Discovery of a Giant Lyα Emitter Near the Reionization Epoch
AU - Ouchi, Masami
AU - Ono, Yoshiaki
AU - Egami, Eiichi
AU - Saito, Tomoki
AU - Oguri, Masamune
AU - McCarthy, Patrick J.
AU - Farrah, Duncan
AU - Kashikawa, Nobunari
AU - Momcheva, Ivelina
AU - Shimasaku, Kazuhiro
AU - Nakanishi, Kouichiro
AU - Furusawa, Hisanori
AU - Akiyama, Masayuki
AU - Dunlop, James S.
AU - Mortier, Angela M. J.
AU - Okamura, Sadanori
AU - Hayashi, Masao
AU - Cirasuolo, Michele
AU - Dressler, Alan
AU - Iye, Masanori
AU - Jarvis, Matt J.
AU - Kodama, Tadayuki
AU - Martin, Crystal L.
AU - McLure, Ross J.
AU - Ohta, Kouji
AU - Yamada, Toru
AU - Yoshida, Michitoshi
PY - 2009/5/1
Y1 - 2009/5/1
N2 - We report the discovery of a giant Lyα emitter (LAE) with a
Spitzer/Infrared Array Camera (IRAC) counterpart near the reionization
epoch at z = 6.595. The giant LAE is found from the extensive 1
deg2 Subaru narrowband survey for z = 6.6 LAEs in the
Subaru/XMM-Newton Deep Survey (SXDS) field, and subsequently identified
by deep spectroscopy of Keck/DEIMOS and Magellan/IMACS. Among our 207
LAE candidates, this LAE is not only the brightest narrowband object
with L(Lyα) = 3.9 ± 0.2 × 1043 erg
s-1 in our survey volume of 106 Mpc3,
but also a spatially extended Lyα nebula with the largest
isophotal area whose major axis is at least sime3''. This object is more
likely to be a large Lyα nebula with a size of gsim17 kpc than to
be a strongly lensed galaxy by a foreground object. Our Keck spectrum
with medium-high spectral and spatial resolutions suggests that the
velocity width is v FWHM = 251 ± 21 km s-1,
and that the line-center velocity changes by sime60 km s-1 in
a 10 kpc range. The stellar mass and star formation rate are estimated
to be 0.9-5.0 × 1010 M sun and >34 M
sun yr-1, respectively, from the combination of
deep optical to infrared images of Subaru, UKIDSS-Ultra Deep Survey, and
Spitzer/IRAC. Although the nature of this object is not yet clearly
understood, this could be an important object for studying cooling
clouds accreting onto a massive halo, or forming-massive galaxies with
significant outflows contributing to cosmic reionization and metal
enrichment of intergalactic medium.
Some of the data presented herein were obtained at the W.M. Keck
Observatory, which is operated as a scientific partnership among the
California Institute of Technology, the University of California, and
the National Aeronautics and Space Administration. The Observatory was
made possible by the generous financial support of the W.M. Keck
Foundation.
AB - We report the discovery of a giant Lyα emitter (LAE) with a
Spitzer/Infrared Array Camera (IRAC) counterpart near the reionization
epoch at z = 6.595. The giant LAE is found from the extensive 1
deg2 Subaru narrowband survey for z = 6.6 LAEs in the
Subaru/XMM-Newton Deep Survey (SXDS) field, and subsequently identified
by deep spectroscopy of Keck/DEIMOS and Magellan/IMACS. Among our 207
LAE candidates, this LAE is not only the brightest narrowband object
with L(Lyα) = 3.9 ± 0.2 × 1043 erg
s-1 in our survey volume of 106 Mpc3,
but also a spatially extended Lyα nebula with the largest
isophotal area whose major axis is at least sime3''. This object is more
likely to be a large Lyα nebula with a size of gsim17 kpc than to
be a strongly lensed galaxy by a foreground object. Our Keck spectrum
with medium-high spectral and spatial resolutions suggests that the
velocity width is v FWHM = 251 ± 21 km s-1,
and that the line-center velocity changes by sime60 km s-1 in
a 10 kpc range. The stellar mass and star formation rate are estimated
to be 0.9-5.0 × 1010 M sun and >34 M
sun yr-1, respectively, from the combination of
deep optical to infrared images of Subaru, UKIDSS-Ultra Deep Survey, and
Spitzer/IRAC. Although the nature of this object is not yet clearly
understood, this could be an important object for studying cooling
clouds accreting onto a massive halo, or forming-massive galaxies with
significant outflows contributing to cosmic reionization and metal
enrichment of intergalactic medium.
Some of the data presented herein were obtained at the W.M. Keck
Observatory, which is operated as a scientific partnership among the
California Institute of Technology, the University of California, and
the National Aeronautics and Space Administration. The Observatory was
made possible by the generous financial support of the W.M. Keck
Foundation.
UR - http://www.scopus.com/inward/record.url?scp=70549095454&partnerID=8YFLogxK
U2 - 10.1088/0004-637X/696/2/1164
DO - 10.1088/0004-637X/696/2/1164
M3 - Article
SN - 1538-4357
VL - 696
SP - 1164
EP - 1175
JO - Astrophysical Journal
JF - Astrophysical Journal
ER -