bluuebunny/crossref_metadata_2025_split huggingface dataset:
FOCAS: The Faint Object Camera and Spectrograph for the Subaru Telescope
Authors: Kashikawa Nobunari , Aoki Kentaro , Asai Ryo , Ebizuka Noboru , Inata Motoko , Iye Masanori , Kawabata Koji S. , Kosugi George , Ohyama Youichi , Okita Kiichi , Ozawa Tomohiko , Saito Yoshihiko , Sasaki Toshiyuki , Sekiguchi Kazuhiro , Shimizu Yasuhiro , Taguchi Hiroko , Takata Tadafumi , Yadoumaru Yasushi , Yoshida Michitoshi 
Published: March 2014

Abstract
The Faint Object Camera and Spectrograph (FOCAS) is a Cassegrain optical instrument for the Subaru Telescope. Its capabilities include $6^\prime \phi$ FOV direct imaging, low-resolution spectroscopy ($R=250 \hbox{--} 2000$ with ${0\rlap {.}{}^{\mathrm {\prime \prime }}4}$ slitwidth), multi-slit spectroscopy and polarimetry. We describe the overall design of FOCAS, its observing functions, and the performance verification procedures that have been carried out.
High Dispersion Spectrograph (HDS) for the Subaru Telescope
Authors: Noguchi Kunio , Aoki Wako , Kawanomoto Satoshi , Ando Hiroyasu , Honda Satoshi , Izumiura Hideyuki , Kambe Eiji , Okita Kiichi , Sadakane Kozo , Sato Bun’ei , Tajitsu Akito , Takada-Hidai Masahide , Tanaka Wataru , Watanabe Etsuji , Yoshida Michitoshi 
Published: March 2014

Abstract
We present the design and performance of the High Dispersion Spectrograph (HDS) of the Subaru Telescope. HDS is an echelle spectrograph located at the Nasmyth focus of the telescope. The collimated beam size is 272 mm, and the echelle is 300 mm by 840 mm in total size ($31.6 \,\mathrm{gr} \,\mathrm{mm}^{-1}, R=2.8$). HDS has two cross-dispersing gratings with $400 \,\mathrm{gr} \,\mathrm{mm}^{-1}$ and $250 \,\mathrm{gr} \,\mathrm{mm}^{-1}$, which are optimized for the blue and red wavelength regions, respectively. The camera is of the catadioptric type system, consisting of three corrector lenses and a mirror. Two EEV-CCD’s with $4100 \times 2048$ pixels and a pixel size of 13.5 ${\mu \mathrm {m}}$ are used as the detector. A standard configuration with a ${0\rlap {.}{}^{\mathrm {\prime \prime }}4}$ slit gives a spectral resolution of $R=90000$, and a narrower slit width enables higher resolution of up to $R \sim 160000$. The spectrograph has sensitivities from 3000 ${Å}$ to 1 ${\mu \mathrm {m}}$, and one exposure covers a range of 1500–2500 ${Å}$, depending on the wavelength region. The throughput of the telescope and the spectrograph, including the efficiency of the detector, is about 13% in 5000–6000 ${Å}$ and about 8% at 4000 ${Å}$. The stability of the spectrograph and scattered light level are also reported.
Development of Iodine Cells for the Subaru HDS and the Okayama HIDES: II. New Software for Precise Radial Velocity Measurements
Authors: Sato Bun’ei , Kambe Eiji , Takeda Yoichi , Izumiura Hideyuki , Ando Hiroyasu 
Published: March 2014

Abstract
We have developed a computer code for precise measurements of stellar radial velocity variations with iodine ($\mathrm{I}_2$) cells attached to the High Dispersion Spectrograph (HDS) on Subaru Telescope and the HIgh Dispersion Echelle Spectrograph (HIDES) on Okayama 188 cm reflector. Our modeling technique for $\mathrm{I}_2$ data is similar to those described by Butler et al. (1996, AAA 65.036.447) and Valenti et al. (1995, AAA 64.036.209) concerning the point that the stellar spectrum taken through the $\mathrm{I}_2$ cell (star$+ \mathrm{I}_2$ spectrum) is modeled as the product of high-resolution stellar and $\mathrm{I}_2$ template spectra convolved with the modeled instrumental profile (IP) of the spectrograph. In order to generate a template stellar spectrum, we have devised a new method to extract an intrinsic stellar spectrum from observed star$+ \mathrm{I}_2$ spectra. This enables us to obtain a well-established template stellar spectrum even in cases when the IP and the wavelength scale are apt to vary with time and the observational conditions, and the existing method which reconstructs the IP from a B-star$+ \mathrm{I}_2$ spectrum (Butler et al. 1996; Endl et al. 2000, A&A, 362, 585) fails. We here report on the results of our Doppler measurements of three solar-type stars, 16 Cyg B, $\tau$ Cet, and $\upsilon$ And, based on data collected with HDS and HIDES for about one year. These results show that we have achieved a precision of about $5 \hbox{--} 6 \,\mathrm{m} \,\mathrm{s}^{-1}$ over a time span of one year with our current analysis package with both spectrographs.
Candidates for Intracluster Planetary Nebulae in the Virgo Cluster Based on the Suprime-Cam Narrow-Band Imaging in [O III] and $\mathrm{H}\alpha$
Authors: Okamura Sadanori , Yasuda Naoki , Arnaboldi Magda , Freeman Kenneth C. , Ando Hiroyasu , Doi Mamoru , Furusawa Hisanori , Gerhard Ortwin , Hamabe Masaru , Kimura Masahiko , Kajino Toshitaka , Komiyama Yutaka , Miyazaki Satoshi , Nakata Fumiaki , Napolitano Nicola R. , Ouchi Masami , Pannella Maurilio , Sekiguchi Maki , Shimasaku Kazuhiro , Yagi Masafumi 
Published: March 2014

Abstract
We have identified 38 candidates of intracluster planetary nebulae (ICPNe) in a $34^\prime\times27^\prime$ field in the core of the Virgo cluster based on Suprime-Cam imaging through two narrow-band filters centered at redshifted wavelengths of the [O III] $\lambda=5007 \,$$\,{Å}$ and the $\mathrm{H}\alpha \lambda = 6563 \,$$\,{Å}$ lines. Broad-band images in the $V$ and $R$ bands are used to check for any emissions in the adjacent continuum. We describe the method briefly and present a list of the intracluster planetary nebula candidates, together with their finding charts. The ICPN candidates show a highly inhomogeneous distribution, which may suggest an association with the M 86–M 84 subcluster. The fraction of diffuse intracluster light with respect to the total light in galaxies is estimated to be about 10%, leading to an estimate of about 20% for the baryon fraction. A spectroscopic follow up and a wider survey are critical to reveal the nature of the intracluster stellar population.
Aperture Synthesis CO(J=1—0) Observations and Near-Infrared Photometry of the Non-Barred Seyfert Galaxy NGC 5033
Authors: Kohno Kotaro , Vila-Vilaró Baltasar , Sakamoto Seiichi , Kawabe Ryohei , Ishizuki Sumio , Matsushita Satoki 
Published: March 2014

Abstract
Aperture synthesis observations of CO($J = 1 \hbox{-} 0$) emission and near-infrared broad-band photometry of the non-barred Seyfert galaxy NGC 5033 ($D = 18.7 \,\mathrm{Mpc}$) were performed. Our ${3\rlap {.}{}^{\mathrm {\prime \prime }}9} \times {3\rlap {.}{}^{\mathrm {\prime \prime }}6}$ resolution CO observations reveal a perturbed distribution and the kinematics of molecular gas in the center of NGC 5033; we find the characteristic gaseous features that are widely observed in barred spiral galaxies, such as two bright CO peaks near the center (separated by $\sim 3^{\prime\prime}$ or 270 pc from the nucleus), two offset ridges of CO emission emanating from the CO peaks, and a CO ring (with a radius of $\sim 14^{\prime\prime}$ or 1.3 kpc). Double-peaked velocity profiles are also evident near the two CO peaks, implying that these CO peaks are orbit crowding zones in a barred/oval potential. Although NIR data only give an upper limit of the possible bar lengths due to a large inclination of the NGC 5033 disk ($i = 68^{\circ}$), our CO data clearly suggests the presence of a small (the semi-major axis of about $12^{\prime\prime} \hbox{-} 15^{\prime\prime}$ or 1.1–1.4 kpc) nuclear bar (or oval structure) in the center of the “non-barred” galaxy NGC 5033. Our results demonstrate that high-resolution CO imaging-spectroscopy is useful to search for nuclear bars, even in highly inclined systems where isophoto fitting techniques are not applicable. We find that the gas mass-to-dynamical mass ratio, $M_\mathrm{gas}/M_\mathrm{dyn}$, is small ($\leq 1\%$) within a radius of $2^{\prime\prime}$ or 180 pc, in contrast to starburst nuclei. This implies that the starburst does not cohabitate in the type-1.5 Seyfert nucleus of NGC 5033.
Black Hole-Bulge Relation for Narrow-Line Objects
Authors: Bian Wei-Hao , Zhao Yong-Heng 
Published: March 2014

Abstract
It has been thought that narrow-line Seyfert 1 galaxies are likely to be in the early stages of the evolution of active galaxies. To test this suggestion, the ratios of the central massive black hole (MBH) mass to the bulge mass ($M_{\mathrm{bh}} / M_{\mathrm{bulge}}$) were estimated for 22 Narrow Line AGNs (NL AGNs). It is found that NL AGNs appear to have genuinely lower MBH/Bulge mass ratio ($M_{\mathrm{bh}} / M_{\mathrm{bulge}}$). The mean $\log (M_{\mathrm{bh}}/M_{\mathrm{bulge}})$ for 22 NL AGNs is $-3.9 \pm 0.07$, which is an order of magnitude lower than that for Broad Line AGNs and quiescent galaxies. We suggest a nonlinear MBH/Bulge relation and find there exists a relation between the $M_{\mathrm{bh}} / M_{\mathrm{bulge}}$ and the velocity dispersion, $\sigma$, derived from the [O iii] width. A scenario of MBH growth for NL AGNs is one of our interpretations of the nonlinear MBH/Bulge relation. The MBH growth timescales for 22 NL AGNs were calculated, with a mean value $(1.29 \pm 0.24) \times 10^8 \,\mathrm{yr}$. Another plausible interpretation is also possible: that NL AGNs occur in low-$M_{\mathrm{bulge}}$ galaxies and that in such galaxies $M_{\mathrm{bh}} / M_{\mathrm{bulge}}$ is lower than that in galaxies with a higher $M_{\mathrm{bulge}}$, if we consider that NL AGNs already have their “final” $M_{\mathrm{bh}} / M_{\mathrm{bulge}}$. More information of the bulge in NL AGNs is needed to clarify the black hole-bulge relation.
Greenhouse Effect of Cloudy Accretion Disks
Authors: Kitabatake Etsuko , Fukue Jun 
Published: March 2014

Abstract
When an accretion disk is not naked, but covered with an optically-thick cloud, mutual irradiation between the disk and the cloud layer becomes important. We calculated the temperature distribution and the continuous spectra of the clouds as well as the disk. The temperature distribution of the cloud becomes somewhat flat in the central region, and gradually decreases in the outer part, while that of the disk is greatly enhanced, compared with the initial standard disk. The continuous spectrum emitted from the clouds is also modified, and resembles a blackbody spectrum with a single temperature, compared with the disk blackbody spectrum.
Orbital Period Studies of Three Algols: TW And, RW Leo, and AY Vul
Authors: Shengbang Qian 
Published: March 2014

Abstract
The changes in the orbital periods of three EA-type eclipsing binaries, TW And, RW Leo, and AY Vul, are discussed based on an analysis of their $O-C$ curves. For RW Leo, its orbital period was revised and, assuming a cyclic oscillation in the orbital period, a period of 38.4 yr was determined. For the other two systems, TW And and AY Vul, their $O-C$ diagrams show complex variations. Under the assumption of periodic oscillation, cyclic changes with periods of 56.4 and 78.6 yr were discovered to superimpose on upward parabolic changes, indicating a secular period increase. The secular period increases for the two binary systems indicate that they are on an active phase of mass transfer. Assuming the oscillations in the periods to be caused by light-time effects due to the presence of “third bodies” rotating around these binary stars, the orbital parameters of the third bodies were determined. For RW Leo, it is possible to detect an additional third body photometrically and spectroscopically. However, for the other two systems, TW And and AY Vul, it is less likely to see additional bodies, unless the orbital inclination is very small (i.e., $i^{\prime}&lt;30^{\circ}$). New photometric and spectroscopic observations and a careful analysis of those data are needed to check the presence of third bodies.
TRACE Observation of an Arcade Flare Showing Evidence Supporting Quadruple Magnetic Source Model for Arcade Flares
Authors: Uchida Yutaka , Title Alan , Kubo Masahito , Tanaka Tomohiro , Morita Satoshi , Hirose Shigenobu 
Published: March 2014

Abstract
The result of analyses of an arcade flare on 1999 July 19, observed by the Satellite TRACE, is reported, and the significance of the following findings is stressed. It is clearly seen that four magnetic regions of alternating polarities [named A($+$), B($-$), C($+$), and D($-$) from the East in the flaring region] are involved in this arcade flare event in an essential way. The high structure covering the triangular region between A and the northern part of D disappears when the dark filament lying between B and C erupts. The X-ray arcade is formed only between B and C. The overlying structure connecting regions A and the northern part of D disappears and the entire region is involved in the flare. Low-lying loops connect the inner sources to the outer sources. The field lines from regions B to A and C to D are not much affected by the eruption of the dark filament, itself, but the loops near the upper surfaces of the closed loop regions are clearly seen to move toward each other (from both sides to the central line) as the arcade flare progresses between the inner pair, B and C; some of them appear to be converted into a flare arcade. The observed behavior can best be understood in terms of the quadruple magnetic source model advocated by one of the authors (YU). The long-conceived “reclosing of once opened bipolar magnetic arcade” models by the rising dark filament (called CSHKP model) find it difficult to explain this.
The Virgo High-Resolution CO Survey: II. Rotation Curves and Dynamical Mass Distributions
Authors: Sofue Yoshiaki , Koda Jin , Nakanishi Hiroyuki , Onodera Sachiko 
Published: March 2014

Abstract
Based on a high-resolution CO survey of Virgo spirals with the Nobeyama Millimeter-wave Array, we determined the dynamical centers using velocity fields, and derived position–velocity diagrams (PVDs) along the major axes of the galaxies across their dynamical centers. We applied a new iteration method to derive rotation curves (RCs), which reproduce the observed PVDs. The obtained high-accuracy RCs generally show a steep rise in the central $\sim 100$ to 200 pc regions, followed by flat rotation in the disk. We applied a deconvolution method to calculate the surface-mass density (SMD) using the RCs based on two extreme assumptions that the mass distribution is either spherical or thin-disk shaped. Both assumptions give nearly identical results, agreeing with each other within a factor of two at any radii. The SMD distributions revealed central massive cores with peak SMD of $\sim 10^4 \hbox{--} 10^5 \,{{{M}_{\odot}}} \,\mathrm{pc}^{-2}$ and a total mass within 200 pc radius of the order of $\sim 10^9 \,{{{M}_{\odot}}}$. A correlation analysis among the derived parameters shows that the central CO-line intensity is positively correlated with the central SMD, which suggests that the deeper is the gravitational potential, the higher is the molecular gas concentration in the nuclei, regardless of the morphological types.
Biasing and Genus Statistics of Dark Matter Halos in the Hubble Volume Simulation
Authors: Hikage Chiaki , Taruya Atsushi , Suto Yasushi 
Published: March 2014

Abstract
We present a numerical analysis of genus statistics for dark matter halo catalogs from the Hubble volume simulation. The huge box-size of the Hubble volume simulation enables us to carry out a reliable statistical analysis of the biasing properties of halos at a Gaussian smoothing scale of $R_\mathrm{G} \ge 30 \,h^{-1} \,\mathrm{Mpc}$ with a cluster-mass scale of between $7\times 10^{13} \,h^{-1} \,{{{M}_{\odot}}}$ and $6\times 10^{15} \,h^{-1} \,{{{M}_{\odot}}}$. A detailed comparison of the genus for dark matter halos with that for the mass distribution shows that the non-Gaussianity induced by the halo biasing is comparable to that by nonlinear gravitational evolution, and both the shape and the amplitude of the genus are almost insensitive to the halo mass at $R_\mathrm{G} \ge 30 \,h^{-1} \,\mathrm{Mpc}$. In order to characterize the biasing effect on the genus, we apply a perturbative formula developed by Matsubara (1994, AAA 062.161.289). We find that the perturbative formula well describes the simulated halo genus at $R_\mathrm{G} \ge 50\,h^{-1} \,\mathrm{Mpc}$. The result indicates that the biasing effect on the halo genus is well approximated by nonlinear deterministic biasing up to the second-order term in the mass density fluctuation. The two parameters describing the linear and quadratic terms in the nonlinear biasing accurately specify the genus for galaxy clusters.
Characteristic Variability Time Scales of Long Gamma-Ray Bursts
Authors: Shen Rong-Feng , Song Li-Ming 
Published: March 2014

Abstract
We determined the characteristic variability time scales (${\Delta t}_\mathrm{p}$) of 410 bright and long GRBs, by locating the peaks of their Power Density Spectra, defined and calculated in the time domain. We found that the averaged variability time scale decreases with the peak flux. This is consistent with the time-dilation effect expected for the cosmological origin of GRBs. We also found that the occurrence distribution of the characteristic variability time scale shows bimodality, which might be interpreted as that the long GRB sample is composed of two sub-classes with different variability time scales. However, we found no difference for some other characteristics of these two sub-classes.
Lyman Break Galaxies at z ∼ 5: Luminosity Function
Authors: Iwata Ikuru , Ohta Kouji , Tamura Naoyuki , Ando Masataka , Wada Shinpei , Watanabe Chisato , Akiyama Masayuki , Aoki Kentaro 
Published: March 2014

Abstract
We present the results of a search for Lyman break galaxies (LBGs) at $z \sim 5$ in a 618 square-arcmin field including the Hubble Deep Field-North (HDF-N) taken by the Subaru Prime Focus Camera. Utilizing the published redshift data of the HDF-N and its flanking fields, the color selection criteria were chosen so that LBGs could be picked out most efficiently and least contaminated by foreground objects. The numbers of detected LBG candidates were 96 in $23.0 \leq I_c \; (\mathrm{mag}) \leq 24.5$ and 310 in $23.0 \leq I_c \leq 25.5$. There is a hint of a deficiency of bright blue galaxies, although it is not as clear as has been suggested for LBGs at $z \sim 3$ to 4. With 305 LBG candidates in a 575 square-arcmin field, the rest-frame UV luminosity function of LBGs at $4.4 \lesssim z \lesssim 5.3$ was derived statistically by considering both the contamination by objects at the intermediate redshift and the incompleteness of the survey. The fraction of the contamination was estimated to be $\sim 50 \%$ in the faintest magnitude range. The completeness of the survey was $\sim 80\%$ at the bright part of the sample, and $\sim 20\%$ in the faintest magnitude range ($25.0 &lt; I_c \leq 25.5$). The luminosity function of LBG candidates at $z \sim 5$ did not show a significant difference from those of LBGs at $z \sim 3$ and 4, though there might be a slight decrease in the fainter part. The UV luminosity density within the observational limit was 0.56–0.69 times smaller than that obtained for LBGs at $z \sim 3$, depending on the adopted cosmology and the integration range of the luminosity function. This decrease in the UV luminosity at $z \sim 5$ compared to that at $z \sim 3$ is due to the smaller number density of faint galaxies at $z \sim 5$. The similarity of the luminosity functions at redshifts 5 to 3 implies that most of the LBGs at $z \sim 5$ should have faded out at $z \sim 3$, and that the LBGs at $z \sim 5$ are different galaxies from those seen at $z \sim 3$, if we take the face values for the ages of the LBGs at $z \sim 3$ obtained by a SED fitting in which a continuous star formation in an individual galaxy was assumed. However, if the star formation in LBGs is sporadic, the similarity of the luminosity function at $z \sim 3$ and 5 would be explained. Such sporadic star formation has been suggested by hydrodynamical simulations and semi-analytic models with collisional starbursts, and the trend of the cosmic star formation history predicted by these studies resembles that estimated from an integration of the UV luminosity density within the observational limit.
Photon Emission in a Cascade from Relativistic Protons Initiated by Residual Thermal Photons in Gamma-Ray Bursts
Authors: Asano Katsuaki , Takahara Fumio 
Published: March 2014

Abstract
Gamma-ray bursts are generally considered to be the result of internal shocks generated in an inhomogeneous relativistic outflow that arises from a fireball. In such shocks, the Fermi acceleration of protons is naturally expected to be at least as efficient as that of electrons. We investigate the consequences of proton acceleration in the residual thermal photon field of a fireball, especially those on the emission spectra of photons. In contrast to most other studies, we do not invoke a direct electron acceleration in shock waves. We show that the residual radiation field of the fireball can ignite the photopion production and subsequent cascade, and that the photons emitted in this process further enhance the photon-initiated cascade. We find that Fermi-accelerated protons with $\gtrsim 10^{13} \,\mathrm{eV}$ efficiently bring their energy into pion production and subsequent photon emission. The particles cascading from the pions emit photons over a wide energy range. The photons emitted from electron–positron pairs distribute continuously from the GeV range down to the X-ray range, while muons can emit gamma-rays by synchrotron radiation with a break at around 1–10 MeV. We also discuss several radiation processes which may possibly produce a break feature in the MeV range, as observed in addition to muon synchrotron radiation.
Parent Distributions of the Periods and Magnetic Inclination Angles of Radio Pulsars
Authors: Zhang Li , Jiang Ze-Jun , Mei Dong-Cheng 
Published: March 2014

Abstract
We studied the parent distributions of pulsar periods and inclination angles by means of the Monte Carlo method. In our simulations, assuming that the parent period distribution satisfies a gamma function with two parameters, we tested a number of various parent distributions of the inclination angles ($\alpha$), which are the inclination angles of the magnetic axis to the pulsar spin axis, and different relations between the beam angular radius ($\rho$) and the pulsar period ($P$) (i.e. $\rho \hbox{-} P$ relation). The simulated periods, pulse widths, and inclination angles were compared with the observed data using the Kolmogorov–Smirnov significance test. Our results indicate that: (i) the parent inclination angles could not be expressed by a flat function (a possible parent distribution is cosine-like or $\propto \{ 0.6/ \cosh[ 3.5 (\alpha-0.43) ] \} + \{ 0.15 / \cosh[ 4.0 (\alpha-1.6) ] \}$); (ii) the parent period distribution depends slightly on the $\rho \hbox{-} P$ relation, and is different from the observed period distribution (their differences can be expressed by different values of two parameters when the parent and observed period distributions can be described as gamma functions); and (iii) the average beaming fraction is about 0.12.
Meteor Storm Activity and Average Size of Meteoroids for the 2001 Leonids by FM Broadcasting Radio Observation
Authors: Yoshida Hideto 
Published: March 2014

Abstract
Radio-wave observations using FM broadcasting frequencies have been performed on the 2001 Leonids. The observations were designed so that only a long echo could be received. The following results were obtained. First, the peak activity of the 2001 Leonids was approximately 18h10m (UT) on November 18 and the solar longitude of this peak corresponded to ${236\rlap {.}{}^{\mathrm {\circ }}45}$ (J2000.0). Second, it is inferred that the peak activity of the 2001 Leonids (1699 and 1866 dust trails) contained meteoroids of a larger average size than those of the 1999 Leonids (1899 dust trail).