18 research outputs found
Subaru Observations for the K-band Luminosity Distribution of Galaxies in Clusters near to 3C 324 at z1.2
We investigate the -band luminosity distribution of galaxies in the region
of clusters at near to the radio galaxy 3C 324. The imaging data
were obtained during the commissioning period of the Subaru telescope. There is
a significant excess of the surface number density of the galaxies with
17--20 mag in the region within 40'' from 3C 324. At this bright end,
the measured luminosity distribution shows a drop, which can be represented by
the exponential cut off of the Schechter-function formula; the best-fitted
value of the characteristic magnitude, , is . This
measurement follows the evolutionary trend of the of the rich clusters
observed at an intermediate redshift, which is consistent with passive
evolution models with a formation redshift z_f \gtsim 2. At K \gtsim 20
mag, however, the excess of the galaxy surface density in the region of the
clusters decreases abruptly, which may imply that the luminosity function of
the cluster galaxies has a negative slope at the faint end. This may imply
strong luminosity segregation between the inner and outer parts of the
clusters, or some deficit of faint galaxies in the cluster central region of
the cluster.Comment: 12 pages, 9 figures, accepted for publication in PAS
H Emission Nebulosity Associated with KH 15D
An H emission filament is found in close proximity to the unique object
KH 15D using the adaptive optics system of the Subaru Telescope. The morphology
of the filament, the presence of spectroscopic outflow signatures observed by
Hamilton et al., and the detection of extended H emission from KH 15D by
Deming, Charbonneau, & Harrington suggest that this filament arises from
shocked H in an outflow. The filament extends about 15" to the north of KH
15D.Comment: 11 pages, 3 figures, 1 table. Astrophysical Journal Letters, in pres
Near-Infrared Adaptive Optics Spectroscopy of Binary Brown Dwarf HD 130948B and C
We present near-infrared spectroscopy of low-mass companions in a nearby
triple system HD 130948 (Gliese 564, HR 5534). Adaptive optics on the Subaru
Telescope allowed spectroscopy of the individual components of the 0".13 binary
system. Based on a direct comparison with a series of template spectra, we
determined the spectral types of HD 130948B and C to be L4 +- 1. If we take the
young age of the primary star into account (0.3-0.8 Gyr), HD 130948B and C most
likely are a binary brown dwarf system.Comment: 6 pages, 3 figures, accepted for publication in ApJ Letter
A Subarcsecond Companion to the T Tauri Star AS 353B
Adaptive optics imaging of the bright visual T Tauri binary AS 353 with the
Subaru Telescope shows that it is a hierarchical triple system. The secondary
component, located 5.6" south of AS 353A, is resolved into a subarcsecond
binary, AS 353Ba and Bb, separated by 0.24". Resolved spectroscopy of the two
close components shows that both have nearly identical spectral types of about
M1.5. Whereas AS 353A and Ba show clear evidence for an infrared excess, AS
353Bb does not. We discuss the possible role of multiplicity in launching the
large Herbig-Haro flow associated with AS 353A.Comment: AASTeXv5.0, 21 pages, 5 figures, Astronomical Journal, in pres
Direct Observation of the Extended Molecular Atmosphere of o Cet by Differential Spectral Imaging with an Adaptive Optics System
We present new measurements of the diameter of o Cet (Mira) as a function of
wavelength in the 2.2 micron atmospheric window using the adaptive optics
system and the infrared camera and spectrograph mounted on the Subaru
Telescope. We found that the angular size of the star at the wavelengths of CO
and H2O absorption lines were up to twice as large as the continuum
photosphere. This size difference is attributable to the optically thick CO and
H2O molecular layers surrounding the photosphere. This measurement is the first
direct differential spectroscopic imaging of stellar extension that resolves
individual molecular lines with high spectral-resolution observations. This
observation technique is extremely sensitive to differences in spatial profiles
at different wavelengths; we show that a difference in diameter much smaller
than the point spread function can be measured.Comment: 6 pages, 3 figures, accepted for publication in PAS
First Detection of NaI D lines in High-Redshift Damped Lyman-alpha Systems
A Near-infrared (1.18-1.35 micron) high-resolution spectrum of the
gravitationally-lensed QSO APM 08279+5255 was obtained with the IRCS mounted on
the Subaru Telescope using the AO system. We detected strong NaI D 5891,5897
doublet absorption in high-redshift DLAs at z=1.062 and 1.181, confirming the
presence of NaI, which was first reported for the rest-frame UV NaI
3303.3,3303.9 doublet by Petitjean et al. This is the first detection of NaI D
absorption in a high-redshift (z>1) DLA. In addition, we detected a new NaI
component in the z=1.062 DLA and four new components in the z=1.181 DLA. Using
an empirical relationship between NaI and HI column density, we found that all
"components" have large HI column density, so that each component is classified
as DLA absorption. We also detected strong NaI D absorption associated with a
MgII system at z=1.173. Because no other metal absorption lines were detected
in this system at the velocity of the NaI absorption in previously reported
optical spectra (observed 3.6 years ago), we interpret this NaI absorption
cloud probably appeared in the line of sight toward the QSO after the optical
observation. This newly found cloud is likely to be a DLA based upon its large
estimated HI column density. We found that the N(NaI)/N(CaII) ratios in these
DLAs are systematically smaller than those observed in the Galaxy; they are
more consistent with the ratios seen in the Large Magellanic Cloud. This is
consistent with dust depletion generally being smaller in lower metallicity
environments. However, all five clouds of the z=1.181 system have a high
N(NaI)/N(CaII) ratio, which is characteristic of cold dense gas. We tentatively
suggest that the host galaxy of this system may be the most significant
contributor to the gravitational-lens toward APM 08279+5255.Comment: 22 pages, 6 Postscript figures, 3 tables, ApJ in press (Vol.643, 2
June 2006
Current Performance and On-Going Improvements of the 8.2 m Subaru Telescope
An overview of the current status of the 8.2 m Subaru Telescope constructed
and operated at Mauna Kea, Hawaii, by the National Astronomical Observatory of
Japan is presented. The basic design concept and the verified performance of
the telescope system are described. Also given are the status of the instrument
package offered to the astronomical community, the status of operation, and
some of the future plans. The status of the telescope reported in a number of
SPIE papers as of the summer of 2002 are incorporated with some updates
included as of 2004 February. However, readers are encouraged to check the most
updated status of the telescope through the home page,
http://subarutelescope.org/index.html, and/or the direct contact with the
observatory staff.Comment: 18 pages (17 pages in published version), 29 figures (GIF format),
This is the version before the galley proo
Spatially Resolved 3 um Spectroscopy of IRAS 22272+5435: Formation and Evolution of Aliphatic Hydrocarbon Dust in Proto-Planetary Nebula
We present medium-resolution 3 um spectroscopy of the carbon-rich
proto-planetary nebula IRAS 22272+5435. Spectroscopy with the Subaru Telescope
adaptive optics system revealed a spatial variation of hydrocarbon molecules
and dust surrounding the star. The ro-vibrational bands of acetylene (C2H2) and
hydrogen cyanide (HCN) at 3.0 um are evident in the central star spectra. The
molecules are concentrated in the compact region near the center. The 3.3 and
3.4 um emission of aromatic and aliphatic hydrocarbons is detected at 600--1300
AU from the central star. The separation of spatial distribution between gas
and dust suggests that the small hydrocarbon molecules are indeed the source of
solid material, and that the gas leftover from the grain formation is being
observed near the central star. The intensity of aliphatic hydrocarbon emission
relative to the aromatic hydrocarbon emission decreases with distance from the
central star. The spectral variation is well matched to that of a laboratory
analog thermally annealed with different temperatures. We suggest that either
the thermal process after the formation of a grain or the variation in the
temperature in the dust-forming region over time determines the chemical
composition of the hydrocarbon dust around the proto-planetary nebula.Comment: 14 pages, 7 figures, Accepted for publication in the Astrophyical
Journa