bluuebunny/crossref_metadata_2025_split huggingface dataset:
The 1996–1997 Fading of V651 Monocerotis, the Binary Central Star of the Planetary Nebula NGC 2346
Authors: Kato Taichi , Nogami Daisaku , Baba Hajime 
Published: March 2014

Abstract
V651 Mon is the binary central star of the bipolar planetary nebula NGC 2346. The star showed the second-ever deep fading in 1996–1997, which was presumably caused by obscuration by a dust cloud in the planetary nebula, as was proposed to explain the 1981–1985 event. The entire duration of the 1996–1997 event was $\sim 400 \,\mathrm{d}$, remarkably shorter than the 1981–1985 event, suggesting that the obscuring body was smaller or had a larger tangential velocity. The most remarkable feature in this event was the presence of a sharply defined transient clearing (brightening). From the time-scale of the variation, we propose an upper limit of the projected scale of several times $\sim 10^{11} \,\mathrm{cm}$ of the structure responsible for the brightening. This observation provides the first evidence for a sharply defined, small lucent structure within the obscuring body around the central star of NGC 2346.
A 350 GHz SIS Receiver on the Nobeyama 10 m Submillimeter Telescope
Authors: Sekimoto Yutaro , Sakai Takeshi , Saito Gaku , Tatematsu Ken’ichi , Tanaka Kunihiko , Kohno Kotaro , Noguchi Takashi , Iwashita Hiroyuki , Takahashi Toshikazu , Satou Naohisa , Yokogawa Sozo , Sakamoto Seiichi , Ukita Nobuharu , Kawabe Ryohei , Ito Tetsuya , Maezawa Hiroyuki , Yamamoto Satoshi 
Published: March 2014

Abstract
We have developed a low-noise submillimeter-wave SIS receiver (320–360 GHz) for a 10 m submillimeter telescope, which was installed at Nobeyama in 2000 February. This receiver and a millimeter-wave SIS receiver are mounted on the ceiling of the Cassegrain receiver cabin of the 10 m telescope. Two curved mirrors couple a shaped Cassegrain beam from the subreflector to mixer horns. The minimum noise temperature measured in front of the receiver was 52 K in double sideband (DSB) at a local oscillator (LO) frequency of 354 GHz, which corresponds to three-times quantum limits ($3h\nu/k_{\mathrm{B}}$). This noise temperature contributions are resolved into the optics, mixer, and IF parts. The temperature ripple of a two-stage Gifford–McMahon cryocooler has been reduced to be 2 mK peak-to-peak at the mixer block with a helium pot temperature stabilizer. Mechanical vibration (30 ${\mu \mathrm {m}}$ peak-to-peak) of the cold head degrades the receiver stability.
A Survey for High-Latitude Molecular Clouds toward Infrared-Excess Clouds with NANTEN
Authors: Onishi Toshikazu , Yoshikawa Nao , Yamamoto Hiroaki , Kawamura Akiko , Mizuno Akira , Fukui Yasuo 
Published: March 2014

Abstract
A survey for high Galactic latitude molecular clouds was carried out toward the far-infrared-excess clouds of Reach et al. (1998, AAA 070.131.207) using the NANTEN telescope. All 68 infrared-excess clouds that are observable from NANTEN were mapped in the $J = 1 \hbox{--} 0$ line of 12CO. CO emission was detected from 32 infrared excess clouds, corresponding to a CO detection rate of 47%. Most of these CO clouds were identified and mapped as high-latitude clouds for the first time. The CO detection rate for the cold ($T_\mathrm{dust} \lt 17 \,\mathrm{K}$) infrared excess clouds is 72%, which is more than a factor of two higher than that of warmer ones, 33%. This indicates that the cold clouds are well shielded from external UV radiation, resulting in a high CO abundance and a low temperature of the clouds. The infrared-excess clouds with no CO emission are most likely to be molecular hydrogen clouds because the temperature is similar to, or lower than, that of the surrounding H i gas. The molecular gas without CO emission seems to occupy more than 90% of the area of the infrared-excess clouds.
A Large-Scale Study of H13CO+ and C18 (J=1–0) in Orion B
Authors: Aoyama Hiroko , Mizuno Norikazu , Yamamoto Hiroaki , Onishi Toshikazu , Mizuno Akira , Fukui Yasuo 
Published: March 2014

Abstract
We have made a new survey for dense cloud cores in the Orion B region using the NANTEN telescope. Two molecular transitions, the $J = 1 - 0$ line of $\mathrm{H}{{13\atop} \mathrm{CO}}^{+}$ and the $J = 1 - 0$ line of $\mathrm{C}{{18\atop} \mathrm{O}}$, were used to study the distribution of dense molecular gas with densities of $10^{4} - 10^{5} \,\mathrm{cm}^{-3}$. We detected 19 $\mathrm{C}{{18\atop} \mathrm{O}}$ clumps, and the mass and the size of the $\mathrm{C}{{18\atop} \mathrm{O}}$ clumps ranged from 13${M}_{\odot}$ to 990${M}_{\odot}$ and from 0.26 pc to 0.69 pc, respectively. Among the physical parameters of these $\mathrm{C}{{18\atop} \mathrm{O}}$ clumps, the molecular column density, $N(\mathrm{H}_2)$, has been found to be the best indicator of star formation; the molecular column density averaged within a $\mathrm{C}{{18\atop} \mathrm{O}}$ clump shows a good correlation with the IRAS luminosity as $L_\mathrm{IRAS} / {{{L}_{\odot}}} \propto N(\mathrm{H}_{2}) \; (\mathrm{cm}^{-2})^{4.8 \pm 0.6}$ (C.C.$= 0.96$). We also detected 11 $\mathrm{H}{{13\atop} \mathrm{CO}}^{+}$ clumps, whose mass ranges from a few ${M}_{\odot}$ to 480${M}_{\odot}$. Five of the $\mathrm{H}{{13\atop} \mathrm{CO}}^{+}$ clumps are of smaller mass, and show no indication of massive star formation; they were newly found in this survey. Five of the eleven $\mathrm{H}{{13\atop} \mathrm{CO}}^{+}$ clumps are particularly massive with an average mass of $\sim 200 \,{{{M}_{\odot}}}$. It is found that these massive $\mathrm{H}{{13\atop} \mathrm{CO}}^{+}$ clumps exhibit active formation of massive stars, as indicated by associated protostellar IRAS point sources, whose luminosities are $10^{2} - 10^{4} \,{{{L}_{\odot}}}$.
A Large Scale 12CO (J=1−0) Survey toward the Chamaeleon Region with NANTEN
Authors: Mizuno Akira , Yamaguchi Reiko , Tachihara Kengo , Toyoda Shuichiro , Aoyama Hiroko , Yamamoto Hiroaki , Onishi Toshikazu , Fukui Yasuo 
Published: March 2014

Abstract
We carried out a large-scale survey for molecular clouds in 12CO ($J = 1-0$) emission toward the Chamaeleon region with the NANTEN 4-meter radio telescope at Las Campanas Observatory in Chile. The survey covered $\sim 491 \,\mathrm{deg}^2$ toward $284 {{}^{\circ }} \lesssim l \lesssim 320 {{}^{\circ }}$ and $-34 {{}^{\circ }} \lesssim b \lesssim-6 {{}^{\circ }}$ at an $8^{\prime}$ grid spacing. The total molecular mass in the observed area is estimated to be $\sim 8300 \,{{{M}_{\odot}}}$. More than 60% of the total mass is concentrated in and around the previously known Cha I, II, and III dark clouds. Two cloud complexes having molecular hydrogen masses of $\sim 430 \,{{{M}_{\odot}}}$ and $\sim 1300 \,{{{M}_{\odot}}}$, respectively, have been found at $\sim 10 {{}^{\circ }}$ galactic-east of the Chamaeleon major clouds. We have identified a prominent filament extending from Cha I to the galactic-east direction, which is remarkably long ($\gtrsim 40 \,\mathrm{pc}$) compared with filamentary features found in other dark-cloud complexes. A correlation study between the CO distribution and isolated X-ray emitting T Tauri stars (TTSs) indicates that $\gtrsim 65\%$ of the TTSs are located within 1 pc of the 12CO cloud boundaries. This suggests that low-density parental molecular gas still remains around the isolated TTSs, although the dense parts with density greater than $10^3 \,\mathrm{cm}^{-3}$ have almost dissipated. This provides further support for the local formation of “isolated” T Tauri stars in small clouds.
CO Column Density and Extinction in the Chamaeleon II–III Dark-Cloud Complex
Authors: Hayakawa Takahiro , Cambrésy Laurent , Onishi Toshikazu , Mizuno Akira , Fukui Yasuo 
Published: March 2014

Abstract
We carried out 13CO ($J = 1 - 0$) and $\mathrm{C}{{18\atop} \mathrm{O}}$ ($J = 1 - 0$) observations of the Chamaeleon II-III dark-cloud complex with the NANTEN radio telescope. The column densities of both molecular isotopes were derived assuming LTE. The $A_{V}$ values were obtained by scaling the $A_{J}$ values that were derived using an adaptive-grid star-count method applied to the DENIS $J$-band data. We established the $A_{V}-$CO isotope column-density relations in Cha II and III, and compared them with those in Cha I. The slopes of the $A_{V}$-13CO relations for Cha II and III are steeper than that for Cha I. Those of the $A_{V} - \mathrm{C}{{18\atop} \mathrm{O}}$ relations are similar among the three clouds. The total column density ratio, $N({{13\atop} \mathrm{CO}})/N(\mathrm{C}{{18\atop} \mathrm{O}})$, in Cha I tends to be small compared with those in Cha II or Cha III; the ratios range from $\sim 5$ to $\sim 25$ at low extinction in Cha II and III, but at most $\sim 10$ in Cha I. We suggest that the increase of $N({{13\atop} \mathrm{C}}{{\atop} \mathrm{O}})$ due to the ${{13\atop} \mathrm{C}}{{\atop} \mathrm{O}}$ formation process causes cloud-to-cloud variations in the $A_{V} - N({{13\atop} \mathrm{C}}{{\atop} \mathrm{O}})$ correlation.
ASCA Observation of the Nearest Gravitational Lensing Cluster Candidate — A 3408
Authors: Katayama Haruyoshi , Hayashida Kiyoshi , Hashimotodani Kiyoshi 
Published: March 2014

Abstract
We observed the nearest gravitational lensing cluster candidate, A 3408 ($z = 0.042$), with ASCA. The projected mass profile of A 3408 was determined from the ICM temperature and the $\beta$-model parameters obtained with ASCA, assuming that the hot gas is spherically symmetric and in hydrostatic equilibrium. The projected mass within an arc radius, $r_\mathrm{arc}$, of 110 kpc is $M(r_\mathrm{arc}) = 1.2^{+0.8}_{-0.4} \times10^{13} \,{{{M}_{\odot}}}$. This is 18–45% of the mass previously derived from a lensing analysis by Campusano et al. (1998, AAA 069.160.189) without any X-ray information.
The primary cause of this discrepancy is in their assumption that the center of the cluster potential coincides with the position of the brightest cluster galaxy (BCG), while we reveal the BCG position to be $60^{\prime\prime}$ outside of the X-ray center. We further calculated a model for the source galaxy position and the gravitational potential that can reproduce both the X-ray data and the arc image. In this model, the magnification factor of the lens for the source galaxy was evaluated to be $\Delta m = 0.07 \pm 0.03 \,\mathrm{mag}$; i.e., the source galaxy is slightly magnified by the lens cluster A 3408.
An Abundance Study in the Hg-Mn Star 46 Aquilae (HD 186122) with the SUBARU/HDS
Authors: Sadakane Kozo , Takada-Hidai Masahide , Takeda Yoichi , Ando Hiroyasu , Aoki Wako , Honda Satoshi , Izumiura Hideyuki , Kajino Toshitaka , Kambe Eiji , Kawanomoto Satoshi , Noguchi Kunio , Okita Kiichi , Sato Bun’ei , Watanabe Etsuji 
Published: March 2014

Abstract
A detailed abundance analysis has been carried out for the Hg-Mn star 46 Aql using high-resolution spectra in the visual region (5100–6400 ${Å}$) obtained with the High Dispersion Spectrograph of the Subaru Telescope. Our attention has been mainly focused on those elements which have not been analyzed previously. He, C, N, and O are underabundant, while Na shows the solar abundance. We have confirmed previously reported underabundances of Mg, Al, and Si, and have found an overabundances of P ($+1.5\,\mathrm{dex}$) and Ti ($+1.0 \,\mathrm{dex}$) and a significant underabundance of S ($-1.8 \,\mathrm{dex}$). Fe is overabundant by $+0.8 \pm 0.1 \,\mathrm{dex}$ and a microturbulent velocity of $0.3 \,\mathrm{km} \,\mathrm{s}^{-1}$ was found from an analysis of the Fe ii lines. Among a few hundred unidentified absorption lines, we identified lines of As ii and Xe ii and a very large ($+4.0 \,\mathrm{dex}$) overabundance of Xe is obtained. We have confirmed emission lines of Mn ii and Ti ii near 6100 ${Å}$, while those of Cr ii cannot have been seen.
First Results of a CO Survey of the Small Magellanic Cloud with NANTEN
Authors: Mizuno Norikazu , Rubio Mónica , Mizuno Akira , Yamaguchi Reiko , Onishi Toshikazu , Fukui Yasuo 
Published: March 2014

Abstract
We present the first results from a new 12CO ($J = 1 \hbox{--} 0$) survey of the Small Magellanic Cloud (SMC) with the NANTEN millimeter-wave telescope. The survey covered the northeast and southwest regions of the main Bar, and the H ii regions N 84, N 88 in the Wing at a linear resolution of $\sim 50 \,\mathrm{pc}$. Twenty-one giant molecular clouds (GMCs), whose masses are $\sim 10^{4} \hbox{--} 10^{6} \,{{{M}_{\odot}}}$, were identified. Significant CO emission, $T_\mathrm{R}^{\ast} \sim 0.36 \,\mathrm{K}$, was first detected toward the N 84 region in the Wing, which is comparable to those of the prominent CO clouds associated with infrared sources LIRS 36, LIRS 49 in the Bar. The GMCs exhibit a good spatial correlation with the H ii regions and young clusters, indicating that cluster formation is on-going in these GMCs. On the other hand, they show little correlation with older clusters or with supernova remnants, suggesting rapid dissipation of CO.
α Element Abundances in Mildly Metal-Poor Stars
Authors: Qiu Hong-Mei , Zhao Gang , Takada-Hidai Masahide , Chen Yu-Qin , Takeda Yoichi , Noguchi Kunio , Sadakane Kozo , Aoki Wako 
Published: March 2014

Abstract
We present [O/Fe] and other $\alpha$-elements/Fe ratios in a sample of 24 mildly metal-poor stars. The sample stars are thought to be brighter than 9.0 magnitude and have available $\mathit{uvby}$ photometric data. Also, based on the typical LTE abundance analysis, we find that [Si/Fe] and [Ca/Fe] are correlated with each other. Combining the kinematic data and the metallicity, we can classify the sample stars into three groups. An abundance analysis shows some evidence that these groups are chemically discrete from each other. Further, the general trend of a decreasing overabundance of the $\alpha$ elements with increasing metallicity has been confirmed.
Centrally Peaked X-Ray Supernova Remnants in the Small Magellanic Cloud Studied with ASCA and ROSAT
Authors: Yokogawa Jun , Imanishi Kensuke , Koyama Katsuji , Nishiuchi Mamiko , Mizuno Norikazu 
Published: March 2014

Abstract
This paper presents ASCA/SIS and ROSAT/HRI results of three supernova remnants (SNRs) in the Small Magellanic Cloud: 0103$-$726, 0045$-$734, and 0057$-$7226. The ROSAT/HRI images of these SNRs indicate that the most of the X-ray emissions are concentrated in the center region. Only from 0103$-$726 are faint X-rays along the radio shell also detected. The ASCA/SIS spectra of 0103$-$726 and 0045$-$734 exhibit strong emission lines from highly ionized metals. The spectra were well-fitted with non-equilibrium ionization (NEI) plasma models. The metal abundances are found to be larger than the mean chemical compositions in the interstellar medium (ISM) of the SMC. Thus, X-rays from these two SNRs are attributable to the ejecta gas, although the ages estimated from the ionization timescale are significantly large, $\gtrsim 10^4 \,\mathrm{yr}$. The chemical compositions are roughly consistent with the type-II supernova origin of a progenitor mass $\lesssim 20 \,{{{M}_{\odot}}}$. The SIS spectrum of 0057$-$7226 was also fitted with an NEI model of an estimated age $\gtrsim 6 \times 10^3 \,\mathrm{yr}$. Although no constraint on the metal abundances was obtained, the rather weak emission lines are consistent with the low metal abundances in the ISM of the SMC. A possible scenario for the evolution of the morphologies and spectra of SNRs is proposed.
The Variability Mechanism of Seyfert Galaxy NGC 4151
Authors: Fan Jun-Hui , Su Cheng-Yue , Lin Rui-Guang 
Published: March 2014

Abstract
Based on compilation by Fan and Su (1998, AAA 70.158.417), the variability property is discussed for the Seyfert galaxy NGC 4151 using the structure function, $ V(\tau)^{\frac{1}{2}} \sim \tau^{k}$. The derived $ k$ is $ 0.35 \pm 0.03$, suggesting that the disk-instability favors the star-burst model as an explanation for the mechanism of the variability in this source.
Kilo-Second Quasi-Periodic Oscillations in the Cataclysmic Variable DW Cancri
Authors: Uemura Makoto , Kato Taichi , Ishioka Ryoko , Novak Rudolf , Pietz Jochen 
Published: March 2014

Abstract
Our photometric monitoring revealed that DW Cnc, which was originally classified as a dwarf nova ($ V=15 \hbox{--} 17.5$), remained at a bright state of $ R_\mathrm{c}=14.68\pm 0.07$ for 61 days. In conjunction with optical spectra lacking a strong He II emission line, we propose that the object is not a dwarf nova, but a non-magnetic nova-like variable. Throughout our monitoring, the object showed strong quasi-periodic oscillations (QPOs) with amplitudes reaching about 0.3 mag. Our period analysis yielded a power spectrum with two peaks of QPOs, whose center periods are $ 37.5\pm 0.1$ and $ 73.4\pm 0.4 \,\mathrm{min}$ and, furthermore, with a significant power in frequencies lower than the QPOs. DW Cnc is a unique cataclysmic variable in which kilo-second QPOs were continuously detected for 61 days. We propose two possible interpretations of DW Cnc: (i) A permanent superhumper below the period minimum of hydrogen-rich cataclysmic variables. (ii) A nova-like variable having an orbital period over 3 hours. In this case, the QPOs may be caused by trapped disk oscillations.
Study of the X-Ray Background Spectrum and Its Large-Scale Fluctuation with ASCA
Authors: Kushino Akihiro , Ishisaki Yoshitaka , Morita Umeyo , Yamasaki Noriko Y. , Ishida Manabu , Ohashi Takaya , Ueda Yoshihiro 
Published: March 2014

Abstract
We studied the energy spectrum and the large-scale fluctuation of the X-ray background with the ASCA GIS instrument based on the ASCA Medium Sensitivity Survey and Large Sky Survey observations. A total of 91 fields with Galactic latitude $|b| \gt 10^\circ$ were selected with a sky coverage of 50 deg$^2$ and 4.2 Ms of exposure. For each field, non-X-ray events were carefully subtracted and sources brighter than $\sim 2\times 10^{-13} \,\mathrm{erg} \,\mathrm{cm}^{-2} \,\mathrm{s}^{-1}$ (2–10 keV) were eliminated. Spectral fits with a single power-law model for the individual 0.7–10 keV spectra showed a significant excess below $\sim 2 \,\mathrm{keV}$, which could be expressed by an additional thermal model with $kT\simeq 0.4 \,\mathrm{keV}$ or a steep power-law model with a photon index of $\Gamma^\mathrm{soft}\simeq 6$. The 0.5–2 keV intensities of the soft thermal component varied significantly from field to field by $1\,\sigma= 52^{+4}_{-5}\%$, and showed a maximum toward the Galactic Center. This component is considered to be entirely Galactic. As for the hard power-law component, an average photon index of 91 fields was obtained to be $\Gamma^\mathrm{hard} = 1.412\pm 0.007\pm 0.025$ and the average 2–10 keV intensity was calculated as $F_\mathrm{X}^\mathrm{hard} = (6.38\pm 0.04\pm 0.64)\times 10^{-8} \,\mathrm{erg} \,\mathrm{cm}^{-2} \,\mathrm{s}^{-1} \,\mathrm{sr}^{-1}$ ($1\,\sigma$ statistical and systematic errors). The Galactic component is marginally detected in the hard band. The 2–10 keV intensities show a $1\,\sigma$ deviation of $6.49^{+0.56}_{-0.61}\%$, while deviation due to the reproducibility of the particle background is 3.2%. The observed deviation can be explained by the Poisson noise of the source count in the f.o.v. ($\sim 0.5 \,\mathrm{deg}^2$), even assuming a single $\log{N} \hbox{--} \log{S}$ relation on the whole sky. Based on the observed fluctuation and the absolute intensity, an acceptable region of the $\log{N} \hbox{--} \log{S}$ relation was derived, showing a consistent feature with the recent Chandra and XMM-Newton results. The fluctuation of the spectral index was also examined; it implied a large amount of hard sources and a substantial variation in the intrinsic source spectra ($\Gamma_\mathrm{S}\simeq 1.1\pm 1.0$).
Detection of Iron Emission in the z = 5.74 QSO SDSSp J104433.04$-$012502.2
Authors: Aoki Kentaro , Murayama Takashi , Denda Kiyomi 
Published: March 2014

Abstract
We obtained near-infrared spectroscopy of the $z = 5.74$ QSO, SDSSp J104433.04$-$012502.2, with the Infrared Camera and Spectrograph of the Subaru Telescope. The redshift of 5.74 corresponds to a cosmological age of 1.0 Gyr for the current $\Lambda$-dominated cosmology. We found a similar strength of the Fe ii (3000–3500 Å) emission lines in SDSSp J104433.04$-$012502.2 as in low-redshift QSOs. This is the highest redshift detection of iron. We subtracted a power-law continuum from the spectrum and fitted model Fe ii emission and the Balmer continuum. The rest equivalent width of Fe ii (3000–3500 Å) is $\sim 30 \,$ Å, which is similar to those of low-redshift QSOs measured in the same manner. The chemical-enrichment models that assume the lifetime of the progenitor of SNe Ia is longer than 1 Gyr predict that weaker Fe ii emission in high-redshift ($z \gt 3$) QSOs than low-redshift ones. However, none of the observed high redshift QSOs show a systematic decrease of Fe ii emission compared with low-redshift QSOs. This may be due to a shorter lifetime of SNe Ia in QSO nuclei than in the solar neighborhood. Another reason for the strong Fe ii emission at $z = 5.74$ may be a longer cosmological age due to a smaller $\Omega _\mathrm{M}$.
Fluence–Hardness Correlation in Gamma-Ray Bursts
Authors: Liang En-Wei , Xie Guang-Zhong 
Published: March 2014

Abstract
We have studied the total fluence, $F_{\mathrm{total}}$, as a function of the hardness ratio, $\mathit{HR}_{32}$, on gamma-ray bursts (GRBs) observed by BATSE, and suggested two subsets of bursts divided by division of $\log\, (F_{\mathrm{total}}) = 4.5 \times \log\, (\mathit{HR}_{32})-8.5$, then investigated correlations between $\mathit{HR}_{32}$ and $F_{\mathrm{total}}$ as well as the distributions of the duration, $T_{90}$, and $\mathit{HR}_{32}$ in the two subsets. The results show that $F_{\mathrm{total}}$ is not correlated with $\mathit{HR}_{32}$ in the entire set of GRBs, while it is in the two subsets, and the division statistically coincides with the division of $T_{90} \sim 2 \,\mathrm{s}$. A brief discussion along with the results seems to support the point that the anti-correlation between $\mathit{HR}_{32}$ and $T_{90}$ is intrinsic.
Chemical Composition of Carbon-Rich, Very Metal-Poor Subgiant LP 625-44 Observed with the Subaru/HDS
Authors: Aoki Wako , Ando Hiroyasu , Honda Satoshi , Iye Masanori , Izumiura Hideyuki , Kajino Toshitaka , Kambe Eiji , Kawanomoto Satoshi , Noguchi Kunio , Okita Kiichi , Sadakane Kozo , Sato Bun’ei , Shelton Ian , Takada-Hidai Masahide , Takeda Yoichi , Watanabe Etsuji , Yoshida Michitoshi 
Published: March 2014

Abstract
We have obtained high-resolution ($R\sim 90000$) spectra of the carbon-and s-process-element-rich, very metal-poor ($\mathrm{[Fe/H]} =-2.7$) subgiant LP 625-44, as well as those of HD 140283 (a metal-poor subgiant with normal abundance ratio) for a comparison, with the High Dispersion Spectrograph (HDS) for the Subaru Telescope for detailed abundance study. The excess of oxygen in LP 625-44 seems to be remarkable (perhaps by nearly a factor 10) compared with that of HD 140283 derived from the O i triplet around 7770 Å, though the oxygen abundance derived from these lines is uncertain. The Na enhancement in LP 625-44 is by about a factor 50, suggesting hydrogen burning in the ${{22\atop} \mathrm{Ne}}$-rich layer in an asymptotic giant branch star which produced the abundance pattern of this object. In our new spectrum of LP 625-44, the Pb i$\lambda$3683 Å line has been detected, confirming the Pb abundance [$\log \epsilon \mathrm{(Pb)} \sim 1.9$] derived from the Pb i$\lambda$4057 Å line by previous work. The abundance ratio of s-process elements at the second peak (e.g., La, Ce, and Nd) to that at the third peak (Pb) in LP 625-44 is significantly higher (by a factor 5) than that in other three s-process element-rich objects recently studied by van Eck et al. Recent theoretical studies have modeled s-process nucleosynthesis in the radiative layer of asymptotic giant branch stars in the inter-pulse phase. The above results mean that these processes produced a large scatter in the abundance ratios, or different processes (e.g., s-process nucleosynthesis during thermal pulses) contributed to heavy elements in the early Galaxy.