bluuebunny/crossref_metadata_2025_split huggingface dataset:
Broad Balmer-Line Absorption in SDSS J172341.10+555340.5
Authors: Aoki Kentaro 
Published: March 2014

Abstract
We present the discovery of Balmer-line absorption from H$\alpha$ to H9 in an iron low-ionizaton broad absorption line (FeLoBAL) quasar, SDSS J172341.10$+$555340.5, by near-infrared spectroscopy with the Cooled Infrared Spectrograph and Camera for OHS (CISCO) attached to the Subaru Telescope. The redshift of the Balmer-line absorption troughs is 2.0530$\ \pm\ $0.0003, and it is blueshifted by 5370 km s$^{-1}$ from the Balmer emission lines. It is more than 4000 km s$^{-1}$ blueshifted from the previously known UV absorption lines. We detected relatively strong (EW$_{\rm rest} =$ 20 Å) [O III] emission lines that are similar to those found in other broad absorption line quasars with Balmer-line absorption. We also derived the column density of neutral hydrogen of 5.2 $\times$ 10$^{17}\ $cm$^{-2}$ by using the curve of growth and taking account of Ly$\alpha$ trapping. We searched for UV absorption lines that had the same redshift with Balmer-line absorption, and found Al III and Fe III absorption lines at $z =$ 2.053 that correspond to previously unidentified absorption lines, and the presence of other blended troughs that were difficult to identify.
Mass Function of Binary Massive Black Holes in Active Galactic Nuclei
Authors: Hayasaki Kimitake , Ueda Yoshihiro , Isobe Naoki 
Published: March 2014

Abstract
If the activity of active galactic nuclei (AGNs) is predominantly induced by major galaxy mergers, then a significant fraction of AGNs should harbor binary massive black holes in their centers. We have studied the mass function of binary massive black holes in nearby AGNs based on the observed AGN black-hole mass function and the theory of evolution of binary massive black holes interacting with a massive circumbinary disk within the framework of the coevolution of massive black holes and their host galaxies. The circumbinary disk is assumed to be steady, axisymmetric, geometrically thin, self-regulated, self-gravitating but nonfragmenting with a fixed fraction of the Eddington accretion rate, which is typically one tenth of the Eddington value. The timescale of orbital decay is then estimated to be $\sim\ $10$^{8}\ $yr for equal mass black holes, being independent of the black-hole mass, semimajor axis, and viscosity parameter, but dependent on the black-hole mass ratio, Eddington ratio, and mass-to-energy conversion efficiency. This makes it possible for any binary massive black holes to merge within the Hubble time under the binary–disk interaction. We find that (1.5%$\ \pm\ $0.6%) of the total number of nearby AGNs for the equal-mass ratio and (1.3%$\ \pm\ $0.5%) for the one-to-ten mass ratio have close binary massive black holes with an orbital period of less than 10 yr in their centers, detectable with ongoing highly sensitive X-ray monitors, such as Monitor of All-sky X-ray Image and/or Swift/Burst Alert Telescope. Assuming that all binary massive black holes have the equal-mass ratio, about 10% of AGNs with black-hole masses of 10$^{6.5-7}\ M_{\odot}$ have close binaries, and thus provide the best chance to detect them.
Astrometry of Galactic Star-Forming Region Onsala 1 with VERA: Estimation of Angular Velocity of Galactic Rotation at the Sun
Authors: Nagayama Takumi , Omodaka Toshihiro , Nakagawa Akiharu , Handa Toshihiro , Honma Mareki , Kobayashi Hideyuki , Kawaguchi Noriyuki , Miyaji Takeshi 
Published: March 2014

Abstract
We conducted the astrometry of H$_2$O masers in the Galactic star-forming region Onsala 1 (ON 1) with the VLBI Exploration of Radio Astrometry (VERA). We measured a trigonometric parallax of 0.404$\ \pm\ $0.017 mas, corresponding to a distance of 2.47$\ \pm\ $0.11 kpc. ON 1 appears to be located near the tangent point at a Galactic longitude of 69$^\circ\!\!\!.$54. We estimated the angular velocity of the Galactic rotation at the Sun (the ratio of the Galactic rotation velocity at the Sun to the distance from the Sun to the Galactic center) to be $\Omega_0$$=$$\Theta_0 / R_0$$=$ 28.7$\ \pm\ $1.3 km s$^{-1}\ $kpc$^{-1}\ $ using the measured distance and proper motion of ON 1. This value is larger than the IAU recommended value of (220 km s$^{-1}/$8.5 kpc) $=$ 25.9 km s$^{-1}\ $ kpc$^{-1}\ $, but consistent with other results recently obtained with the VLBI technique.
Measurement of the Distance and Proper Motions of the H2O Masers in the Young Planetary Nebula K 3−35
Authors: Tafoya Daniel , Imai Hiroshi , GÓmez Yolanda , Torrelles José M. , Patel Nimesh A. , Anglada Guillem , Miranda Luis F. , Honma Mareki , Hirota Tomoya , Miyaji Takeshi 
Published: March 2014

Abstract
In this paper we present the results of very long baseline interferometry (VLBI) observations carried out with the VLBI Exploration of Radio Astrometry (VERA) array and the Very Long Baseline Array (VLBA) toward H$_{2}$O masers in a young planetary nebula K 3$-$35. From the VERA observations we measured the annual parallax and proper motion of a bright water maser spot in K 3$-$35. The resulting distance is $D$$=$ 3.9$^{+0.7}_{\hskip1.11pt-0.5}$ kpc. This is the first time that the parallax of a planetary nebula is obtained by observations of its maser emission. On the other hand, the proper motion of K 3$-$35 as a whole was estimated to be $\mu_{\alpha}$$=$$-$3.34 $\pm$ 0.10 mas yr$^{-1}$, $\mu_{\delta}$$=$$-$5.93 $\pm$ 0.07 mas yr$^{-1}$. From these results we determined the position and velocity of K 3$-$35 in Galactic cylindrical coordinates: ($R,\theta,\textsl{z}$) $=$ (7.11$^{+0.08}_{\hskip1.11pt-0.06}$ kpc, 27$^{\circ}$$\pm$ 5$^{\circ}$, 140$^{+25}_{\hskip1.11pt-18}$ pc) and ($V_{R}, V_{\theta}, V_{{\sl z}}$) $=$ (33 $\pm$ 16, 233 $\pm$ 11, 11 $\pm$ 2) km s$^{-1}$. Additionally, from our VLBA observations we measured the relative proper motions among the water maser spots located in the central region of the nebula, which have been proposed to be tracing a toroidal structure. The distribution and relative proper motions of the masers, compared with previous reported observed epochs, suggest that such structure could be totally destroyed within a few years, due to the action of high-velocity winds and the expansion of the ionization front in the nebula.
Deep CO Observations and the CO-to-H2 Conversion Factor in DDO 154, a Low Metallicity Dwarf Irregular Galaxy
Authors: Komugi Shinya , Yasui Chikako , Kobayashi Naoto , Hatsukade Bunyo , Kohno Kotaro , Sofue Yoshiaki , Kyu Shiori 
Published: March 2014

Abstract
We present a deep spectroscopic search for CO emission in the dwarf irregular galaxy DDO 154, which has an Oxygen abundance of only 1$/$20 of the solar value. The observations were conducted in order to constrain the CO-to-H$_2$ conversion factor at low metallicity. No CO was detected, however, despite being one of the sensitive observations done towards galaxies of this type. We succeed in putting a strong lower limit on the conversion factor, at least 10-times the Galactic value. Our result supports previous studies that argue for a high conversion factor at low metallicity.
Asteroid Catalog Using AKARI: AKARI/IRC Mid-Infrared Asteroid Survey
Authors: Usui Fumihiko , Kuroda Daisuke , MÜLler Thomas G. , Hasegawa Sunao , Ishiguro Masateru , Ootsubo Takafumi , Ishihara Daisuke , Kataza Hirokazu , Takita Satoshi , Oyabu Shinki , Ueno Munetaka , Matsuhara Hideo , Onaka Takashi 
Published: March 2014

Abstract
We present the results of an unbiased asteroid survey in the mid-infrared wavelength region with the Infrared Camera (IRC) on board the Japanese infrared satellite AKARI. About 20% of the point source events recorded in the AKARI All-Sky Survey observations are not used for the IRC Point Source Catalog (IRC-PSC) in its production process because of a lack of multiple detection by position. Asteroids, which are moving objects on the celestial sphere, remain in these ``residual events''. We identify asteroids out of the residual events by matching them with the positions of known asteroids. For the identified asteroids, we calculate the size and albedo based on the Standard Thermal Model. Finally we have a new brand of asteroid catalog, named the Asteroid Catalog Using AKARI (AcuA), which contains 5120 objects, about twice as many as the IRAS asteroid catalog. The catalog objects comprise 4953 main belt asteroids, 58 near-Earth asteroids, and 109 Jovian Trojan asteroids. The catalog is publicly available via the Internet.
Experimental Search for the HAYABUSA Re-Entry Module on the Ground by Using a Remote-Sensing Instrument onboard Formosat-2 Satellite
Authors: Nakamura Ryosuke , Chen Bo , Matsuoka Masashi , Yamamoto Hirokazu , Kamei Akihide , Nakamura Kazuki , Yano Hajime 
Published: March 2014

Abstract
HAYABUSA was the first asteroid sample return mission launched from Uchinoura, Japan in 2003. The sample capsule re-entered the Earth's atmosphere at approximately 13:50 (UT) on 2010 June 13th, and safely landed on the Woomera Prohibited Area (WPA) in Australia. The capsule had to be found and retrieved as soon as possible to reduce any contamination risk. On the morning of the June 13th and 14th, the landing area was imaged by using Remote Sensing Instrument (RSI) onboard the Formosat-2 satellite to locate the HAYABUSA re-entry module, consisting of a capsule and a parachute. In spite of an accurate geometric registration and radiance comparison of the image pair, no statistically significant radiance variation was found on the landing site. It was demonstrated through this experiment, however, that satellite imagery could be a promising backup tool for the prompt discovery and retrieval of the sampling capsule of the HAYABUSA follow-on mission if we can utilize space-borne imagers with sub-meter spatial resolution and short revisit capability.
Star Formation in the Cometary Tails Associated with Cluster Galaxies
Authors: Yamagami Takahiro , Fujita Yutaka 
Published: March 2014

Abstract
We investigate the star-formation in cometary tails of galaxies in clusters. In particular, we focus on the evolution of molecular clouds in the tails that generate the stars. Assuming that the gas tails had been derived from the galaxies through ram-pressure stripping, we found that the gas must have been stripped mostly not in the form of molecular clouds, but in the form of H I gas or molecular gas that is not in clouds. Moreover, the molecular clouds are condensed in the tails, even away from the host galaxies. We also found that magnetic fields may be required to suppress the Kelvin–Helmholtz (KH) instability on the surface of molecular clouds, because otherwise the KH instability may destroy the molecular clouds before stars are formed in them.
Astrometry of 6.7 GHz Methanol Maser toward W 3(OH) with Japanese VLBI Network
Authors: Matsumoto Naoko , Honma Mareki , Isono Yasuko , Ujihara Hideki , Kimura Kimihiro , Matsumoto Kouhei , Sawada-Satoh Satoko , Doi Akihiro , Fujisawa Kenta , Ueno Yuji 
Published: March 2014

Abstract
We present the results of multiepoch VLBI observations for a 6.7 GHz methanol maser toward the UC H II region of W 3(OH) with Japanese VLBI Network (JVN). Based on phase-referencing VLBI astrometry, we derived the trigonometric annual parallax to be 0.598$\ \pm\ $0.067 mas, corresponding to a distance of 1.67$^{+0.21}_{-0.17}$ kpc. This is the first detection of parallax for a 6.7 GHz methanol maser with JVN, and demonstrates that JVN/VERA is capable of conducting VLBI astrometry for 6.7 GHz methanol maser sources within few kpc from the Sun. Based on in-beam mapping of the W 3(OH) methanol maser, we also measured the internal proper motions of its 6.7 GHz methanol maser for the first time. The internal proper motions basically show north–south expansion with a velocity of few km s$^{-1}$, being similar to OH masers. The spatial distribution and the internal proper motions of 6.7 GHz methanol masers suggest a rotating and expanding torus structure surrounding the UC H II region.
Long-Term Monitoring of the Black Hole Binary GX 339−4 in the High/Soft State during the 2010 Outburst with MAXI/GSC
Authors: Shidatsu Megumi , Ueda Yoshihiro , Nakahira Satoshi , Negoro Hitoshi , Yamaoka Kazutaka , Sugizaki Mutsumi , Hiroi Kazuo , Kawai Nobuyuki , Mihara Tatehiro , Matsuoka Masaru , Kimura Masashi , Ishikawa Masaki , Isobe Naoki , Kitayama Hiroki , Kohama Mitsuhiro , Matsumura Takanori , Morii Mikio , Nakagawa Yujin E. , Nakajima Motoki , Serino Motoko , Sootome Tetsuya , Sugimori Kousuke , Suwa Fumitoshi , Toizumi Takahiro , Tomida Hiroshi , Tsuboi Yohko , Tsunemi Hiroshi , Ueno Shiro , Usui Ryuichi , Yamamoto Takayuki , Yamazaki Kyohei , Yoshida Atsumasa 
Published: March 2014

We present the results of monitoring the galactic black hole candidate GX 339 $-$ 4 with the Monitor of All-sky X-ray Image (MAXI) / Gas Slit Camera in the high/soft state during an outburst in 2010. All of the spectra throughout the 8-month period were well reproduced with a model consisting of multi-color disk emission and its Comptonization component, whose fraction is $\leq\ $ 25% in the total flux. In spite of the flux variability over a factor of 3, the innermost disk radius is constant at $R_{\rm in}$ $=$ 61 $\ \pm\ $ 2 km for an inclination angle of $i$ $=$ 46 $^\circ$ and a distance of $d$ $=$ 8 kpc. This $R_{\rm in}$ value is consistent with those of past measurements with Tenma in the high/soft state. Assuming that the disk extends to the innermost stable circular orbit of a non-spinning black hole, we estimate the black hole mass to be $M$ $=$ 6.8 $\ \pm\ $ 0.2 $\ M_{\odot}$ for $i$ $=$ 46 $^\circ$ and $d$ $=$ 8 kpc, which is consistent with that estimated from the Suzaku observation of the previous low/hard state. Further combined with the mass function, we obtained a mass constraint of 4.3 $\ M_\odot$ $&lt;$ $M$ $&lt;$ 13.3 $\ M_\odot$ for the allowed range of $d$ $=$ 6–15 kpc and $i$ $&lt;$ 60 $^\circ$ . We also discuss the spin parameter of the black hole in GX 339 $-$ 4 by applying relativistic accretion disk models to the Swift/XRT data.
Search for X-Ray Emission Associated with the Shapley Supercluster with Suzaku
Authors: Mitsuishi Ikuyuki , Gupta Anjali , Yamasaki Noriko Y. , Takei Yoh , Ohashi Takaya , Sato Kosuke , Galeazzi Massimiliano , Henry J. Patrick , Kelley Richard L. 
Published: March 2014

Suzaku performed observations of 3 regions in and around the Shapley supercluster, a region located between A 3558 and A 3556, at $\sim\ $0.9 times the virial radii of both clusters, and two other regions at 1$^\circ$ and 4$^\circ$ away from the first pointing. The 4$^\circ$-offset observation was used to evaluate the Galactic foreground emission. We did not detect significant redshifted Oxygen emission lines (O VII and O VIII) in the spectra of all three pointings, after subtracting the contribution of foreground and background emission. The upper limit for the redshifted O VIII K$\alpha$ line intensity of the warm-hot intergalactic medium (WHIM) is 1.5 $\times$ 10$^{-7}$ photons s$^{-1}$ cm$^{-2}$ arcmin$^{-2}$, which corresponds to an overdensity of $\sim\ $380 ($Z/$0.1$\ Z_{\odot}$)$^{-1/2}$ ($L/$3 Mpc)$^{-1/2}$, assuming $T$ $=$ 3 $\times$ 10$^{6}$ K. We found excess continuum emission in the 1$^\circ$-offset and on-filament regions, represented by thermal models with $ kT\sim 1$ keV and $\sim\ $2 keV, respectively. The redshifts of both 0 and that of the supercluster (0.048) are consistent with the observed spectra. The $\sim\ $1 keV emission can also be fitted with Ne-rich Galactic (zero redshift) thin thermal emission. The radial intensity profile of the 2 keV component suggests contributions from A 3558 and A 3556, but with significant steepening of the intensity slope in the outer region of A 3558. Finally, we summarized the previous Suzaku search for the WHIM, and discussed the feasibility of constraining the WHIM. An overdensity of $\lt\ $400 could be detectable using O VII and O VIII emission lines in a range of 1.4 $\times$ 10$^{6}$ K $\lt\ $ $T$ $\lt\ $ 5 $\times$ 10$^{6}$ K or a continuum emission in a relatively high-temperature range of $T$ $\gt$ 5 $\times$ 10$^{6}$ K with the Suzaku XIS. The non-detection with Suzaku suggests that a typical line-of-sight average overdensity is $\lt\ $400.
Near-Infrared High-Dispersion Spectroscopic Observations of Water in Comet 81P/Wild 2 with Subaru/IRCS
Authors: Hashimoto Mio , Kobayashi Hitomi , Kawakita Hideyo 
Published: March 2014

Abstract
Near-infrared high-dispersion spectroscopic observations of comet 81P/Wild 2 were carried out on 2010 January 31 and February 1 by the Subaru telescope with IRCS. We detected two hot-band emission lines of H$_{2}$O: X(1,0,1) 2$_{02}$–X(1,0,0) 3$_{03}$ at 3526.5 cm$^{-1}$ and X(1,0,1) 2$_{11}$–X(1,0,0) 3$_{12}$ at 3514.4 cm$^{-1}$. The water production rate (${Q_{\rm H_{2}O}}$) was determined as (1.21 $\pm$ 0.05) ${\times}$ 10$^{28}$ molecules s$^{-1}$ based on the spherical coma model assuming the rotational temperature of 30 K on February 1. We found that water production rates determined by de Val-Borro et al. (2010, A&A, 521, L50) with Herschel/HIFI were consistent with ours within 3 $\sigma$ error-levels. Furthermore, our result is consistent with previous water production rates determined in the 1997 apparition.
NH$_{3}$ Survey Observation of Massive Star-Forming Region W 43
Authors: Nishitani Hiroyuki , Sorai Kazuo , Habe Asao , Hosaka Keita , Watanabe Yoshimasa , Ohishi Yukie , Motogi Kazuhito , Minamidani Tetsuhiro , Fujimoto Masayuki Y. 
Published: March 2014

Abstract
We consider the properties of giant molecular cloud complexes in the star-forming region W 43 with a resolution of several pc scale, and discuss their relations to the evolutionary stages of massive star formation. We performed a NH$_{3}$ ($J$, $K$) $=$ (1, 1), (2, 2), and (3, 3) inversion-line survey with the Hokkaido University 11-m telescope. Among 51 observed positions, selected based on integrated intensity maps of $^{13}$CO ($J$$=$ 1–0), these three emissions were detected from 21, 8, and 5 positions, respectively. The integrated intensity of the NH$_{3}$ ($J$, $K$) $=$ (1, 1) line was found to be proportional to the far-infrared luminosity, estimated from IRAS data. The rotation temperatures were deduced to be $\sim\ $15–20 K at eight observed positions. In addition, the upper limits were estimated for 13 positions, which include the relatively low temperatures below 14 K at two positions with a relatively high fractions of NH$_{3}$ for $^{13}$CO and with a low far-infrared luminosity. We derived the ortho-to-para abundance ratio of NH$_{3}$. From the population distribution between the ortho- and para-levels of NH$_{3}$, we also derived temperatures of $\sim\ $6–12 K, which may be interpreted as the temperatures when NH$_{3}$ molecules were formed. We discuss the relevance of the present results of our observations to the massive star-formation process and the current status of the W 43 region while taking into account previous observations of other indicators of massive star formation. It is shown that the complexes contain several regions in different evolutionary stages, or with the distinct characteristics of star formation within a timescales shorter than the lifetime of massive stars.
On the Error Reduction of a Simple Symplectic Integrator
Authors: Ito Takashi , Tanikawa Kiyotaka 
Published: March 2014

Abstract
An analysis of truncation errors of the simplest symplectic integrator is revisited. We performed an analytical error estimate of this integrator within the framework of a canonical perturbation method, taking the two-body system as an example. Our study was motivated by the desire to remove any confusion in the derivation of this issue in one standard literature along this line of research. We repeated the derivation, and examined how a secular numerical error arises in symplectic integration. We showed that it is possible to substantially eliminate a secular numerical error by choosing appropriate initial conditions, as previous studies have shown. On the other hand, depending on boundary parameter values, such as the eccentricity in the two-body system, we could see that it is sometimes impossible to reduce the secular numerical error by changing the starting conditions. We also numerically demonstrated this reduction, or lack of reduction of numerical errors by taking a restricted three-body system as an example. We confirmed that the so-called “iterative start” of symplectic integrators works in certain systems.
Application of the Titius–Bode Rule to the 55 Cancri System: Tentative Prediction of a Possibly Habitable Planet
Authors: Cuntz Manfred 
Published: March 2014

Abstract
Following the notion that the Titius–Bode rule (TBR) may also be applicable to some extrasolar planetary systems, although this number could be relatively small, it is applied to 55 Cancri, which is a G-type main-sequence star currently known to host five planets. Following a concise computational process, we tentatively identified four new hypothetical planetary positions, given as 0.081, 0.41, 1.51, and 2.95 AU from the star. The likelihood that these positions are occupied by real existing planets is significantly enhanced for the positions of 1.51 and 2.95 AU in view of previous simulations on planet formation and planetary orbital stability. For example, Raymond, Barnes, and Gorelick (2008, ApJ, 689, 478) argued that additional planets would be possible between 55 Cnc f and 55 Cnc d, which would include planets situated at 1.51 and 2.95 AU. If two additional planets are assumed to exist between 55 Cnc f and 55 Cnc d, the deduced domains of stability would be given as 1.3–1.6 and 2.2–3.3 AU. The possible planet near 1.5 AU appears to be located at the outskirts of the stellar habitable zone, which is, however, notably affected by the stellar parameters as well as the adopted model of circumstellar habitability. We also computed the distance of the next possible outer planet in the 55 Cnc system, which, if existing, is predicted to be located between 10.9 and 12.2 AU, which is consistent with orbital stability constraints. The inherent statistical significance of the TBR was evaluated following a method by Lynch (2003, MNRAS, 341, 1174). Yet it is up to future planetary search missions to verify or falsify the applicability of the TBR to the 55 Cnc system, and to obtain information on additional planets, if existing.
Estimates of Emission-Region Locations of Fermi Flat-Spectrum Radio Quasars
Authors: Yan Dahai , Zeng Houdun , Zhang Li 
Published: March 2014

Abstract
We have studied the location of emission regions through modeling the quasi-simultaneous multifrequency spectral energy distributions of 21 Fermi flat-spectrum radio quasars (FSRQs) in the frame of a multicomponent one-zone leptonic model. In our calculations, we took the detailed broad line region (BLR) structure into account, and discussed the effect of the uncertainty of the BLR structure on constraining the location of the emission regions for each FSRQ; besides, we also included both the internal and the external absorptions. Our results indicate that: (1) the contribution of the external Compton-BLR component to the $ \gamma$-ray emission is important, and the energy density of external target-photon fields depends on the location of the emission region, which can be derived by reproducing the observed $ \gamma$-ray emission; (2) the emission regions of FSRQs with relatively low accretion-disk luminosity lie in the region of (7.9 $ \times$ 10$ ^{16}$ –1.3 $ \times$ 10$ ^{18})$ cm (300–4300 Schwarzschild radii) from central black hole, and for FSRQs with high accretion-disk luminosity, the emission regions are located in a larger region of (2.6 $ \times$ 10$ ^{17}$ –4.2 $ \times$ 10$ ^{18}$ ) cm (300–5600 Schwarzschild radii).