bluuebunny/crossref_metadata_2025_split huggingface dataset:
New Photometric Investigation of the G-Type Contact Binary GSC 0763-0572
Authors: Jing-Jing Wang , Sheng-Bang Qian , Er-Gang Zhao , Li-Ying Zhu , Wen-Ping Liao , Kai Li , Jia Zhang , Liang Liu , Lin-Jia Li 
Published: March 2014

Abstract
We present new CCD photometric light curves of the W UMa-type binary system GSC 0763-0572 in the $ V$ , $ R$ , and $ I$ bands. Here, the light curves in the $ R$ and $ I$ bands are the first to be obtained. The primary component of this system belongs to a G-type solar-like star; our new observation indicates that the activities of GSC 0763-0572 may be stable. Based on all available times of the light minimum, we found that the orbital period is variable. The $ O$$-$$ C$ curve suggested that the period of GSC 0763-0572 is undergoing a continuous increase at a rate of $ dP/dt$$ =$$ +$ 5.81(33) $ \times$ 10$ ^{-7}$ d yr$ ^{-1}$ . Photometric solutions were derived by using the Wilson–Devinney code. We confirmed that this system is A-subtype overcontact binary with a degree of contact factor of $ f$$ =$ 31.0% ($ \pm$ 1.5%), a mass ratio of $ q$$ =$ 0.2330, and a temperature difference of $ \Delta{T}$$ =$ 31 K. The long-term increase of the orbital period can be explained by mass transfer from the less-massive component to the more-massive one. It's inferred that GSC 0763-0572 may presently be in an expanding state of thermal relaxation oscillation, and may finally evolve into a rapid-rotating single star.
Detection of Methyl Formate in the Second Torsionally Excited State (υt = 2) in Orion KL
Authors: Takano Shuro , Sakai Yusuke , Kakimoto Suguru , Sasaki Mutsumi , Kobayashi Kaori 
Published: March 2014

Abstract
We report on the detection of rotational transitions of methyl formate (HCOOCH$ _{3}$ ) in the second torsionally excited state ($ v_{\rm t}$$ =$ 2) of the methyl internal rotation in Orion Kleinmann–Low (KL). Recent progress in the microwave spectroscopy of methyl formate in laboratories and sensitive radioastronomical observations have made it possible to assign $ \sim$ 20 emission lines to methyl formate in the $ v_{\rm t}$$ =$ 2 state. The beam-averaged column density obtained with the Nobeyama 45 m radiotelescope is (3.0 $ \pm$ 1.5) $ \times$ 10$ ^{14}$ cm$ ^{-2}$ in this state. In addition to this state, we also observed lines in the ground and the first torsionally excited states ($ v_{\rm t}$$ =$ 0 and 1) in Orion KL. The obtained rotational temperatures for the $ v_{\rm t}$$ =$ 0 and 1 states are 43 $ \pm$ 9 and 53 $ \pm$ 8 K, respectively. The column densities for the $ v_{\rm t}$$ =$ 0 and 1 states are (3.8 $ \pm$ 1.2) $ \times$ 10$ ^{15}$ and (9.8 $ \pm$ 2.3) $ \times$ 10$ ^{14}$ cm$ ^{-2}$ , respectively, which are 13 and 3 times the column density in the $ v_{\rm t}$$ =$ 2 state. Data of these three states can be explained by a single vibrational temperature of 124 $ \pm$ 5 K, which is significantly higher than the rotational temperatures. As excitation mechanisms, there are two possibilities: collision with H$ _2$ and pumping by far-infrared radiation from star-formation activities. Considering the temperature difference and Einstein's $ A$ coefficients of the torsional states, we cannot rule out either of these possibilities. This detection further indicates that many more unidentified lines in Orion KL will be due to low-lying excited states of methyl formate and other organic molecules.
Erratum: X-Ray Study of the Outer Region of Abell 2142 with Suzaku
Authors: Akamatsu Hiroki , Hoshino Akio , Ishisaki Yoshitaka , Ohashi Takaya , Sato Kosuke , Takei Yoh , Ota Naomi 
Published: March 2014

Abstract
In the paper [PASJ 63, S1019 (2012)], there was an error in the estimation of gas mass. The correct gas mass at the virial radius is 2.40$\ \pm\ $0.20 $\times$ 10$^{14}\ M_{\bigodot}$. Thus, the gas mass fraction also changes from 14.4$^{+7.1}_{-4.1}$% to 21.8$^{+10.7}_{-6.3}$%. Although this value is still consistent with the weak-lensing result of $\sim\ $18% (Okabe & Umetsu 2008, PASJ, 60, 345), our result allows possibilities for the low electron temperature compared with that of ions, gas clumpiness in the cluster outskirts as reported in the Perseus cluster (Simionescu et al. 2011, Science, 331, 1576) and non-thermal pressure such as turbulence and bulk motions in ICM (Kawaharada et al. 2010, ApJ, 714, 423). The conclusions in the paper are not affected by this change.
Initial Results from Nobeyama Molecular Gas Observations of Distant Bright Galaxies
Authors: Iono Daisuke , Hatsukade Bunyo , Kohno Kotaro , Kawabe Ryohei , Ikarashi Soh , Ichikawa Kohei , Kodama Tadayuki , Motohara Kentaro , Nakajima Taku , Nakanishi Koichiro , Ohta Kouji , Ota Kazuaki , Saito Toshiki , Suzuki Kenta , Tadaki Ken-ichi , Tamura Yoichi , Ueda Junko , Umehata Hideki , Yabe Kiyoto , Yoshida Tessei , Yuma Suraphong , Kuno Nario , Takano Shuro , Iwashita Hiroyuki , Handa Kazuyuki , Higuchi Aya , Hirota Akihiko , Ishikawa Shinichi , Kimura Kimihiro , Maekawa Jun , Mikoshiba Hiroshi , Miyazawa Chieko , Miyazawa Kazuhiko , Muraoka Kazuyuki , Ogawa Hideo , Onodera Sachiko , Saito Yasufumi , Sakai Takeshi , Takahashi Shigeru , Yun Min S. 
Published: March 2014

Abstract
We present initial results from the CO survey toward high-redshift galaxies using the Nobeyama 45 m telescope. Using a new wide bandwidth spectrometer equipped with a two-beam SIS receiver, we have obtained three new detections of high-redshift (z$=$ 1.6–3.4) submillimeter galaxies (SXDF 1100.001/HXMM02, SDP9, and SDP17), one tentative detection (SDSS J160705$+$533558), and one non-detection (COSMOS-AzTEC1). The galaxies observed during the commissioning phase are sources with known spectroscopic redshifts from previous optical or wide-band submillimeter spectroscopy. The derived molecular gas mass and line widths from Gaussian fits are $\sim$ 10$^{11}\ M_{\odot}$ and 430–530 km s$^{-1}$, respectively, which are consistent with previous CO observations of distant submillimeter galaxies and quasars. The spectrometer, which realizes a maximum of 32 GHz instantaneous bandwidth, will provide new science capabilities at the Nobeyama 45 m telescope, allowing us to determine redshifts of bright submillimeter selected galaxies without any prior redshift information.
Imaging Simulations of the Sunyaev–Zel'dovich Effect for ALMA
Authors: Yamada Kenkichi , Kitayama Tetsu , Takakuwa Shigehisa , Iono Daisuke , Tsutsumi Takahiro , Kohno Kotaro , Takizawa Motokazu , Yoshikawa Kohji , Akahori Takuya , Komatsu Eiichiro , Suto Yasushi , Matsuo Hiroshi , Kawabe Ryohei 
Published: March 2014

Abstract
We present imaging simulations of the Sunyaev–Zel'dovich effect of galaxy clusters for the Atacama Large Millimeter/submillimeter Array (ALMA), including the Atacama Compact Array (ACA). In its most compact configuration at 90 GHz, ALMA will resolve the intracluster medium with an effective angular resolution of 5$ ''$ . It will provide a unique probe of shock fronts and relativistic electrons produced during cluster mergers at high redshifts, that are hard to spatially resolve by current and near-future X-ray detectors. The quality of image reconstruction is poor with the 12 m array alone, but improved significantly by adding ACA; the expected sensitivity of the 12 m array based on the thermal noise is not valid for the Sunyaev–Zel'dovich effect mapping unless accompanied by an ACA observation of at least equal duration. The observations above 100 GHz will become excessively time-consuming owing to the narrower beam size and the higher system temperature. On the other hand, significant improvement of the observing efficiency is expected once Band 1 is implemented in the future.
Suzaku Observations of Unidentified X-Ray Sources toward the Galactic Bulge
Authors: Mori Hideyuki , Maeda Yoshitomo , Ueda Yoshihiro , Dotani Tadayasu , Ishida Manabu 
Published: March 2014

Abstract
We present Suzaku observations of two unidentified sources towards the Galactic bulge, 1RXS J165256.3$-$264503 and 1RXS J174459.5$-$172640, both of which were discovered with the ROSAT All-Sky Survey. We obtained wide-band spectra of these sources above 2 keV for the first time. The X-ray spectrum of 1RXS J165256.3$-$264503 consists of two absorbed thin thermal plasma components with temperatures of 0.7 and 2.4 keV. An RS CVn star, HD 152178, was found within a 90% error circle of the source position. Due to this position coincidence, and an X-ray spectrum analogous to those of other RS CVn binaries, we concluded that 1RXS J165256.3$-$264503 is an RS CVn-type active binary. The X-ray spectrum of 1RXS J174459.5$-$172640 was dominated by continuum emission extending up to $\sim$ 20 keV, which can be explained by an absorbed cutoff power-law or a combination of absorbed multicolor disk-blackbody and Comptonized emission. We inferred that the source is a new Galactic-bulge low-mass X-ray binary (LMXB) with a luminosity of 2 $\times$ 10$^{35}$ erg s$^{-1}$, based on its X-ray spectrum and lightcurve. Hence, 1RXS J174459.5$-$172640 may be an intriguing example of an LMXB in an intermediate state in which X-ray emission mechanisms can be readily explored.
Environmental Dependence of Stellar Mass, Star Formation Rate, Specific Star Formation Rate, and AGN Activity for an Apparent Magnitude Limited Main Galaxy Sample of the SDSS DR7
Authors: Deng Xin-Fa , Wu Ping , Qian Xiao-Xia , Luo Cheng-Hong 
Published: March 2014

Abstract
In this study, we used an apparent magnitude limited Main galaxy sample of the Sloan Digital Sky Survey Data Release 7 (SDSS DR7), and investigated the environmental dependence of stellar mass, the star formation rate (SFR), the specific star formation rate (SSFR, the star formation rate per unit stellar mass) and active galactic nucleus (AGN) activity. To decrease the Malmquist bias, we divided the whole apparent magnitude limited Main galaxy sample into many subsamples with a redshift binning size of $ \Delta{z}$$ =$ 0.01, and analysed the environmental dependence of these properties of subsamples in each redshift bin. It turns out that a strong environmental dependence of the stellar mass, SFR and SSFR could be observed in nearly all redshift bins of the apparent magnitude limited Main galaxy sample, and that in most redshift bins (except for a low redshift region of $ z$$ =$ 0.02 to 0.06), the fraction of AGNs in the sample at low density apparently was larger than that in the sample at high density.
Suzaku Observations of the Hydra A Cluster out to the Virial Radius
Authors: Sato Takuya , Sasaki Toru , Matsushita Kyoko , Sakuma Eri , Sato Kosuke , Fujita Yutaka , Okabe Nobuhiro , Fukazawa Yasushi , Ichikawa Kazuya , Kawaharada Madoka , Nakazawa Kazuhiro , Ohashi Takaya , Ota Naomi , Takizawa Motokazu , Tamura Takayuki 
Published: March 2014

Abstract
We report on Suzaku observations of the northern half of the Hydra A cluster out to $ \sim$ 1.4 Mpc, reaching the virial radius. There are the first Suzaku observations of a medium-size ($ kT$$ \sim$ 3 keV) cluster out to the virial radius. Two observations were conducted, north-west and north-east offsets, which continue in a filament direction and a void direction of the large-scale structure of the Universe, respectively. The X-ray emission and distribution of galaxies elongate in the filament direction. The temperature profiles in the two directions are mostly consistent with each other within the error bars, and drop to 1.5 keV at 1.5 $ r_{500}$ . As observed by Suzaku in hot clusters, the entropy profile becomes flatter beyond $ r_{500}$ , in disagreement with the $ r^{1.1}$ relationship, which is expected from accretion shock heating models. When scaled with the average intracluster medium (ICM) temperature, the entropy profiles of clusters observed with Suzaku are universal, and do not depend on the system mass. The hydrostatic mass values in the void and filament directions are in good agreement, and the Navarro, Frenk, and White universal mass profile represents the hydrostatic mass distribution up to $ \sim$ 2$ r_{500}$ . Beyond $ r_{500}$ , the ratio of the gas mass to the hydrostatic mass exceeds the result of the Wilkinson microwave anisotropy probe, and at $ r_{100}$ , these ratios in the filament and void directions reach 0.4 and 0.3, respectively. We discuss possible deviations from the hydrostatic equilibrium at cluster outskirts. We derived radial profiles of the gas-mass-to-light ratio and the iron-mass-to-light ratio out to the virial radius. Within $ r_{500}$ , the iron-mass-to-light ratio of the Hydra A cluster was compared with those in other clusters observed with Suzaku.
Period Analysis using the Least Absolute Shrinkage and Selection Operator (Lasso)
Authors: Kato Taichi , Uemura Makoto 
Published: March 2014

AbstractWe introduced least absolute shrinkage and selection operator (Lasso) in obtaining periodic signals in unevenly spaced time-series data. A very simple formulation with the combination of a large set of sine and cosine functions has been shown to yield a very robust estimate; also, the peaks in the resultant power spectra were very sharp. We studied the response of Lasso to low signal-to-noise data, asymmetric signals and very closely separated multiple signals. When the length of the observation was sufficiently long, all of them were not serious obstacles to Lasso. We analyzed the 100-year visual observations of $ \delta $ Cep, and obtained a very accurate period of 5.366326(16) d. The error in the period estimation was several times smaller than in the phase dispersion minimization. We also modeled the historical data of R Sct, and obtained a reasonable fit to the data. The model, however, lost its predictive ability after the end of the interval used for modeling, which is probably a result of the chaotic nature of the pulsations of this star. We also provided a sample R code for making this analysis.
High-Resolution Near-Infrared Polarimetry of a Circumstellar Disk around UX Tau A
Authors: Tanii Ryoko , Itoh Yoichi , Kudo Tomoyuki , Hioki Tomonori , Oasa Yumiko , Gupta Ranjan , Sen Asoke K. , Wisniewski John P. , Muto Takayuki , Grady Carol A. , Hashimoto Jun , Fukagawa Misato , Mayama Satoshi , Hornbeck Jeremy , Sitko Michael L. , Russell Ray W. , Werren Chelsea , CurÉ Michel , Currie Thayne , Ohashi Nagayoshi , Okamoto Yoshiko , Momose Munetake , Honda Mitsuhiko , Inutsuka Shu-ichi , Takeuchi Taku , Dong Ruobing , Abe Lyu , Brandner Wolfgang , Brandt Timothy D. , Carson Joseph , Egner Sebastian E. , Feldt Markus , Fukue Tsubasa , Goto Miwa , Guyon Olivier , Hayano Yutaka , Hayashi Masahiko , Hayashi Saeko S. , Henning Thomas , Hodapp Klaus W. , Ishii Miki , Iye Masanori , Janson Markus , Kandori Ryo , Knapp Gillian R. , Kusakabe Nobuhiko , Kuzuhara Masayuki , Matsuo Taro , Mcelwain Michael W. , Miyama Shoken , Morino Jun-ichi , Moro-MartÍn Amaya , Nishimura Tetsuro , Pyo Tae-Soo , Serabyn Eugene , Suto Hiroshi , Suzuki Ryuji , Takami Michihiro , Takato Naruhisa , Terada Hiroshi , Thalmann Christian , Tomono Daigo , Turner Edwin L. , Watanabe Makoto , Yamada Toru , Takami Hideki , Usuda Tomonori , Tamura Motohide 
Published: March 2014

Abstract
We present $ H$-band polarimetric imagery of UX Tau A taken with HiCIAO/AO188 on the Subaru Telescope. UX Tau A has been classified as a pre-transitional disk object, with a gap structure separating its inner and outer disks. Our imagery taken with the 0$ \rlap{\hskip1pt .}''$ 15 (21 AU) radius coronagraphic mask has revealed a strongly polarized circumstellar disk surrounding UX Tau A, which extends to 120 AU, at a spatial resolution of 0$ \rlap{\hskip1pt .}''$ 1 (14 AU). It is inclined by 46$ ^{\circ}$$ \pm$ 2$ ^{\circ}$ , since the west side is nearest. Although SED modeling and sub-millimeter imagery have suggested the presence of a gap in the disk, with the inner edge of the outer disk estimated to be located at 25–30 AU, we detect no evidence of a gap at the limit of our inner working angle (23 AU) at the near-infrared wavelength. We attribute the observed strong polarization (up to 66%) to light scattering by dust grains in the disk. However, neither polarization models of the circumstellar disk based on Rayleigh-scattering nor Mie-scattering approximations were consistent with the observed azimuthal profile of the polarization degrees of the disk. Instead, a geometric optics model of the disk with nonspherical grains with radii of 30 $ \mu$ m is consistent with the observed profile. We suggest that the dust grains have experienced frequent collisional coagulations, and have grown in the circumstellar disk of UX Tau A.
V369 Gem: A New Ellipsoidal Variable System with High-level Chromospheric Activity
Authors: Dal Hasan Ali , Sipahi Esin , ÖZdarcan Orkun 
Published: March 2014

Abstract
In this study, we present BVR photometry of V369 Gem in 2006–2008. We combined our $ V$ data with the data taken from the literature. We analysed all of the data together, and calculated new light elements. General features of the light curves were discussed. The light curves were modelled with the Fourier method, and the Fourier coefficients were calculated. The cos (2$ \theta$ ) term was found to be dominant. The pre-whitened $ V$ light curves demonstrated that stellar spot activity also exists. There are generally two minima in the pre-whitened light curves. Thus, there must be two spotted areas, which are separated by about 180$ ^{\circ}$ from each other. As conclusions, we have remarked for the first time that V369 Gem is an ellipsoidal variable with high-level chromospheric activity.
Slow-Scan Observations with the Infrared Camera (IRC) aboard AKARI
Authors: Takita Satoshi , Ikeda Norio , Kitamura Yoshimi , Ishihara Daisuke , Kataza Hirokazu , Kawamura Akiko , Oyabu Shinki , Ueno Munetaka , Yamamura Issei 
Published: March 2014

Abstract
We present the characterization and calibration of the slow-scan observation mode of the Infrared Camera (IRC) aboard AKARI. The IRC Slow-scan observations were operated at the S9W (9 $ \mu$ m) and L18W (18 $ \mu$ m) bands. We developed a toolkit for data reduction of the IRC Slow-scan observations. We introduced a ``self-pointing reconstruction'' method to improve the positional accuracy to as good as 1$ ''$ . The sizes of the point spread functions were derived to be $ \sim$ 6$ ''$ at the S9W band and $ \sim$ 7$ ''$ at the L18W bands in full width at half maximum. Flux calibrations were achieved with observations of 3 and 4 infrared standard stars at the S9W and L18W bands, respectively. The flux uncertainties are estimated to be better than 20% from comparisons with the AKARI IRC PSC and the WISE preliminary catalog.
NRO M 33 All-Disk Survey of Giant Molecular Clouds (NRO MAGiC). II Dense Gas Formation
Authors: Onodera Sachiko , Kuno Nario , Tosaki Tomoka , Muraoka Kazuyuki , Miura Rie E. , Kohno Kotaro , Nakanishi Kouichiro , Sawada Tsuyoshi , Komugi Shinya , Kaneko Hiroyuki , Hirota Akihiko , Kawabe Ryohei 
Published: March 2014

Abstract
We report the results of our observations of the $ ^{12}$ CO (J$ =$ 1–0) and $ ^{12}$ CO (J$ =$ 3–2) line emission of 74 major giant molecular clouds (GMCs) within the galactocentric distance of 5.1 kpc in the Local Group galaxy M 33. The observations have been conducted as part of the Nobeyama Radio Observatory M 33 All-disk survey of Giant Molecular Clouds project (NRO MAGiC). The spatial resolutions are 80 pc for $ ^{12}$ CO (J$ =$ 1–0) and 100 pc for $ ^{12}$ CO (J$ =$ 3–2). We detect $ ^{12}$ CO (J$ =$ 3–2) emission of 65 GMCs successfully. Furthermore, we find that the correlation between the surface density of the star formation rate, which is derived from a linear combination of H$ \alpha$ and 24 $ \mu$ m emissions, and the $ ^{12}$ CO (J$ =$ 3–2) integrated intensity still holds at this scale. This result shows that the star-forming activity is closely associated with warm and dense gases that are traced with the $ ^{12}$ CO (J$ =$ 3–2) line, even in the scale of GMCs. We also find that the GMCs with a high star-forming activity tend to show a high integrated intensity ratio ($ R_{3-2/1-0}$ ). Moreover, we also observe a mass-dependent trend of $ R_{3-2/1-0}$ for the GMCs with a low star-forming activity. From these results, we speculate that the $ R_{3-2/1-0}$ values of the GMCs with a low star-forming activity mainly depend on the dense gas fraction and not on the temperature, and therefore, the dense gas fraction increases with the mass of GMCs, at least in the GMCs with a low star-forming activity.
Asymmetric Dust Jets and Extended Structure of 22P/Kopff Observed During 2009 Appearance
Authors: Hanayama Hidekazu , Ishiguro Masateru , Watanabe Jun-Ichi , Sarugaku Yuki , Fukushima Hideo , Miyaji Takeshi , Yanagisawa Kenshi , Kuroda Daisuke , Yoshida Michitoshi , Ohta Kouji , Kawai Nobuyuki 
Published: March 2014

Abstract
22P/Kopff images were taken with Multicolor Imaging Telescopes for Survey and Monstrous Explosions (MITSuME) 3ch simultaneous CCD cameras on the Ishigakijima astronomical observatory 105-cm telescope and a 2kCCD camera on the Kiso 105-cm Schmidt telescope from 2009 August to December after the passage of its perihelion on 2009 May 25. We confirmed that the near-nuclear fan-shaped jet structure extended toward the south. Whereas we detected a dust trail structure on the project orbit of the parent nucleus, we could not confirm the obvious neck-line structure. We deduced a pole orientation of ($ \alpha_{\rm pl}$ , $ \delta_{\rm pl}$ ) $ =$ (302$ \pm$ 30, 62$ \pm$ 10) or ($ \alpha_{\rm pl}$ , $ \delta_{\rm pl}$ ) $ =$ (122$ \pm$ 30, $-$ 62 $ \pm$ 10) in the case of prograde or retrograde rotation, based on the fan-shaped jet. In addition, we conducted a model simulation of the dust orbital evolution, and found that the observed dust morphology of the fan-shaped jet and dust trail can well explain the dust emission near the south polar region. Finally, we conclude that the surface of 22P/Kopff is becoming largely dormant, but the polar region is still active, as we saw in the Deep Space 1 image of 19P/Borrelly.
Substellar Companions to Seven Evolved Intermediate-Mass Stars
Authors: Sato Bun'ei , Omiya Masashi , Harakawa Hiroki , Izumiura Hideyuki , Kambe Eiji , Takeda Yoichi , Yoshida Michitoshi , Itoh Yoichi , Ando Hiroyasu , Kokubo Eiichiro , Ida Shigeru 
Published: March 2014

Abstract
We report on the detections of substellar companions orbiting around seven evolved intermediate-mass stars from precise Doppler measurements at Okayama Astrophysical Observatory. $o$ UMa (G4 II-III) is a giant with a mass of 3.1 $M_{\odot}$ , and hosts a planet with a minimum mass of $m_2$ sin $i$$=$ 4.1 $M_{\rm J}$ in an orbit with a period $P$$=$ 1630 d and an eccentricity $e$$=$ 0.13. This is the first planet candidate ($\lt $ 13 $M_{\rm J}$ ) ever discovered around a star more massive than 3 $M_{\odot}$ . $o$ CrB (K0 III) is a 2.1 $M_{\odot}$ giant, and has a planet of $m_2$ sin $i$$=$ 1.5 $M_{\rm J}$ in a 187.8 d orbit with $e$$=$ 0.19. This is one of the least-massive planets ever discovered around an $\sim$ 2 $M_{\odot}$ star. HD 5608 (K0 IV) is an 1.6 $M_{\odot}$ subgiant hosting a planet of $m_2$ sin $i$$=$ 1.4 $M_{\rm J}$ in a 793 d orbit with $e$$=$ 0.19. The star also exhibits a linear velocity trend, suggesting the existence of an outer, more massive companion. 75 Cet (G3 III:) is a 2.5 $M_{\odot}$ giant hosting a planet of $m_2$ sin $i$$=$ 3.0 $M_{\rm J}$ in a 692 d orbit with $e$$=$ 0.12. The star also shows a possible additional periodicity of about 200 d and 1880 d with a velocity amplitude of $\sim$ 7–10 m s$^{-1}$ , although these are not significant at this stage. $\nu $ Oph (K0 III) is a 3.0 $M_{\odot}$ giant, and has two brown-dwarf companions of $m_2$ sin $i$$=$ 24 $M_{\rm J}$ and 27 $M_{\rm J}$ , in orbits with $P$$=$ 530.3 d and 3190 d, and $e$$=$ 0.126 and 0.17, respectively, which were independently announced by Quirrenbach, Reffert, and Bergmann (2011, AIP Conf. Proc. 1331, 102). The ratio of the periods is close to 1:6, suggesting that the companions are in mean motion resonance. We also independently confirmed planets around $\kappa $ CrB (K0 III-IV) and HD 210702 (K1 IV), which were announced by Johnson et al. (2008, ApJ, 675, 784) and Johnson et al. (2007a, ApJ, 665, 785), respectively. All of the orbital parameters we obtained are consistent with the previous results.