bluuebunny/crossref_metadata_2025_split huggingface dataset:
Superhump Development during the 2005 Superoutburst of 1RXS J053234+624755
Authors: Imada Akira , Henden Arne , Kato Taichi , Moritani Yuuki , Sumiyoshi Masanao , Tanada Syunsuke , Omodaka Toshihiro , Ishioka Ryoko , Uemura Makoto , Yanagisawa Kenshi , Nogami Daisaku 
Published: March 2014

Abstract
We report on time-resolved CCD photometry of the 2005 March/April superoutburst of a recently confirmed SU UMa-type dwarf nova, 1RXS J053234+624755. The superoutburst was accompanied by a precursor in which conspicuous superhumps were visible from the second night of the precursor. This is a rare example where superhumps were observed during a precursor. Concerning an estimated mass ratio of 0.07 for the system, the present observations contrast with the well-known Lubow relation. We also found that the superhump period increased as the superoutburst proceeded, despite the fact that the superoutburst showed a precursor. If the superhump-period change is closely related to the disk radius of the superoutburst, systems having a small mass ratio could display an increasing superhump period, even if the superoutburst contains a precursor.
Solar-Radiation Heating Effects on 3200 Phaethon
Authors: Ohtsuka Katsuhito , Nakato Aiko , Nakamura Tomoki , Kinoshita Daisuke , Ito Takashi , Yoshikawa Makoto , Hasegawa Sunao 
Published: March 2014

Abstract
Apollo-type near-Earth asteroid 3200 Phaethon, having a small perihelion distance of $q$$\sim$ 0.14 AU, is classified as F- or B-type, one of subclasses among the C-complex (C-, G-, B-, and F-types) asteroids. The F/B-type asteroids and dehydrated CI and CM carbonaceous chondrites, which are regarded as being linked to each other, underwent a thermal history of high-temperature heatings at more than hundreds of degrees and dehydration for a certain period of time after aqueous alteration in their parent bodies. However, their primary heating mechanism and its timing are less certain and still controversial. We have investigated solar-radiation heating effects on Phaethon at the present planetary-epoch. As a consequence, we have found that the effects on Phaethon, if it is still hydrated, might indeed be a likely candidate for the primary metamorphic heat source. We also found that solar-radiation heating on Phaethon is a function of the latitude, since Phaethon has a highly tilted polar axis. Thus, the northern hemisphere would be selectively more heated than the southern hemisphere. Therefore, we hypothesized that the northern hemisphere, especially the north pole–northern midlatitude region, would be more thermally metamorphosed and dehydrated, if solar-radiation heating is the primary metamorphic heat source of Phaethon. This may provide the latitude-dependent color variations on Phaethon’s surface, although this has not been proven by the existing Phaethon’s spectral data.
The Nature of Unresolved Soft X-Ray Emission from the Galactic Disk
Authors: Masui Kensuke , Mitsuda Kazuhisa , Yamasaki Noriko Y. , Takei Yoh , Kimura Shunsuke , Yoshino Tomotaka , McCammon Dan 
Published: March 2014

Abstract
Although about 40% of the soft X-ray background emission in 0.4 to 1 keV range has extragalactic origins and thus is totally blocked by the galactic absorption in midplane directions, it decreases at most by about 20% in midplane. Suzaku observation of the direction, ($\ell$, $b$) $=$ (235$^\circ$, 0$^\circ$), showed an O vii${\rm K} \alpha$ emission intensity comparable with that of the MBM-12 on cloud Suzaku observation, but revealed a narrow bump peaked at $\sim$0.9 keV. The latter component is partly filling the decrease of the extragalactic component in midplane. The feature can be well represented by a thin thermal emission with a temperature of about 0.8 keV. Because of the high pressure implied for spatially extended hot gas, the emission is likely a sum of unresolved faint sources. We consider a large fraction of the emission originates from faint dM stars. We constructed a model spectrum for spatially unresolved dM stars that consistently explains the observed spectrum and the surface brightness. The model also suggests that the emission from dM stars decreases very rapidly with increasing $b$, and thus that it cannot compensate entirely the decrease of the extragalactic component at $b$$\sim$ 2$^\circ$–10$^\circ$.
Suzaku Observations of SS Cygni in Quiescence and Outburst
Authors: Ishida Manabu , Okada Shunsaku , Hayashi Takayuki , Nakamura Ryoko , Terada Yukikatsu , Mukai Koji , Hamaguchi Kenji 
Published: March 2014

Abstract
We present results from the Suzaku observations of the dwarf nova SS Cyg in quiescence and outburst in 2005 November. The high sensitivity of the HXD PIN and the high spectral resolution of the XIS enabled us to determine the plasma parameters with unprecedented precision. The maximum temperature of the plasma in quiescence, 20.4$^{+4.0}_{-2.6}$(stat)$\pm$3.0(sys)keV, is significantly higher than that in outburst, 6.0$^{+0.2}_{-1.3}$keV. The elemental abundances are close to the solar ones for medium-$Z$ elements (Si, S, Ar), whereas they decline both in lighter and heavier elements, except for that of carbon, which is 2 solar, at least. The solid angle of the reflector subtending over an optically thin thermal plasma is $\Omega^{\rm Q}/(2\pi)$$=$ 1.7$\pm$0.2(stat)$\pm$0.1(sys) in quiescence. A 6.4 keV iron K$\alpha$ line is resolved into narrow and broad components. These facts indicate that both the white dwarf and the accretion disk contribute to the reflection. We consider the standard optically thin boundary layer as being the most plausible picture for the plasma configuration in quiescence. The solid angle of the reflector in outburst, $\Omega^{\rm O}\!\!/(2\pi)$$=$ 0.9$^{+0.5}_{-0.4}$, and a broad 6.4 keV iron line indicate that the reflection in outburst originates from the accretion disk and an equatorial accretion belt. The broad 6.4 keV line suggests that the optically thin thermal plasma is distributed on the accretion disk like solar corona.
Revisit to the Nuclear Spin Temperature of NH$_{3}$ in Comet C/2001 Q4 (NEAT) Based on High-Dispersion Spectra of Cometary NH$_{2}$
Authors: Shinnaka Yoshiharu , Kawakita Hideyo , Kobayashi Hitomi , Kanda Yu-ichi 
Published: March 2014

Abstract
The Ortho-to-Para abundance ratio (OPR) of cometary molecules is considered to be one of primordial characters of comeary ices, which has information concerning their formation. In order to determine the OPR of cometary ammonia (NH$_{3}$), high-dispersion spectra in the optical wavelength region have been the most powerful tool, since NH$_{2}$ is a photo-dissociation product of NH$_{3}$, and NH$_{2}$ has a strong electronic transition in the optical region. Here we present an improved procedure to derive the OPR of NH$_{2}$ (OPR of NH$_{3}$ is derived from that of NH$_{2}$) from the high-dispersion spectra of NH$_{2}$ in comets. We consider (1) the contamination of NH$_{2}$ lines by the C$_{2}$ Swan-band lines, (2) the influence by the telluric absorption lines, and (3) multiple measurements of OPR from different vibronic bands of NH$_{2}$ in the optical region, to achieve a more accurate determination of OPRs than that in previous studies. We applied the new method to the spectrum of comet C/2001 Q4 (NEAT) for which the OPR of NH$_{2}$ was determined in the previous study. The derived OPR of NH$_{2}$ is 3.23$ \pm $0.03, and this is more accurate than before. The OPR of NH$_{3}$ is estimated to be 1.12$ \pm $0.02, which corresponds to a nuclear spin temperature ($T_\mathrm{spin}$) of 30$^{+2}_{-1} $K. The $T_\mathrm{spin}$ value of NH$_{3}$ is basically consistent with the temperature inferred from the mixing ratio of CO with respect to H$_{2}$O found in the same comet.
VLBI Monitoring of 3C 84 (NGC 1275) in Early Phase of the 2005 Outburst
Authors: Nagai Hiroshi , Suzuki Kenta , Asada Keiichi , Kino Motoki , Kameno Seiji , Doi Akihiro , Inoue Makoto , Kataoka Jun , Bach Uwe , Hirota Tomoya , Matsumoto Naoko , Honma Mareki , Kobayashi Hideyuki , Fujisawa Kenta 
Published: March 2014

Abstract
Multi-epoch Very Long Baseline Interferometry (VLBI) study of a sub-pc scale jet of 3C 84 is presented. We carried out 14-epoch VLBI observations during 2006–2009 with the Japanese VLBI Network and the VLBI Exploration of Radio Astrometry, immediately following a radio outburst that began in 2005. We confirmed that the outburst was associated with the central $\sim1$ pc core, accompanying the emergence of a new component. This is striking evidence of the recurrence of jet activity. The new component became brighter during 2008, in contrast to constant $\gamma$-ray emission that was observed with the Fermi Gamma-ray Space Telescope during the same time. We found that the projected speed of the new component was 0.23$ c$ from 2007/297 (2007 October 24) to 2009/114 (2009 April 24). The direction of movement of this component differs from that of the pre-existing component by $\sim $40$^{\circ}$. This was the first measurement of the kinematics of a sub-pc jet in a $\gamma$-ray active phase. A possible detection of jet deceleration and the jet kinematics in connection with the $\gamma$-ray emission is discussed.
The Effectiveness of Mid IR / Far IR Blind, Wide Area, Spectral Surveys in Breaking the Confusion Limit
Authors: Raymond Gwenifer , Isaak Kate G. , Clements Dave , Rykala Adam , Pearson Chris 
Published: March 2014

Abstract
Source confusion defines a practical depth to which to take large-area extragalactic surveys. 3D imaging spectrometers with positional as well as spectral information, however, potentially provide a means by which to use line emission to break the traditional confusion limit. In this paper we present the results of our investigation into the effectiveness of mid/far infrared, wide-area spectroscopic surveys in breaking the confusion limit. We use SAFARI, a FIR imaging Fourier Transform Spectrometer concept for the proposed JAXA-led SPICA mission, as a test case. We generate artificial skies representative of 100 SAFARI footprints and use a fully-automated redshift determination method to retrieve redshifts for both spatially and spectrally confused sources for bright-end and burst mode galaxy evolution models. We find we are able to retrieve accurate redshifts for 38/54% of the brightest spectrally confused sources, with continuum fluxes as much as an order of magnitude below the 120 $\mu$m photometric confusion limit. In addition we also recover accurate redshifts for 38/29% of the second brightest spectrally confused sources. Our results suggest that deep, spectral line surveys with SAFARI can break the traditional photometric confusion limit, and will also not only resolve, but provide redshifts for, a large number of previously inaccessible galaxies. To conclude we discuss some of the limitations of the technique, as well as further work.
Energetic Relations between the Disappearing Solar Filaments and the Associated Flare Arcades
Authors: Morimoto Taro , Kurokawa Hiroki , Shibata Kazunari , Ishii Takako T. 
Published: March 2014

Abstract
We present the temporal and statistical relations between the mechanical energies of disappearing solar filaments and the thermal energies of the associated flare arcades in soft X-rays. Measuring the 3-D velocity fields of 10 eruptive filaments, we calculated their mechanical energy gain rate, $\epsilon_{\rm mc}$, per unit volume and compared it to the thermal energy release rate per unit volume, $\epsilon_{\rm th}$, derived with Yohkoh/SXT data. For the statistical relation, we found a relation that can be approximated as $\epsilon_{\rm th} \propto \epsilon_{\rm mc}^{1.9}$. This relation can be explained by interpreting the energy input to an arcade via the Poynting flux in the magnetic reconnection process and the acceleration of a filament by the Lorentz force. This explanation is also supported by the strong dependence of the observed increase rates of both the thermal and mechanical energy densities on the mean magnetic field strength of the source region. We also investigated their temporal variations, and found that the start time of increase in the mechanical energy of a filament preceded that of the thermal energy of the coronal arcade in some cases. These relations imply that the basic mechanisms that accelerate a filament and create a hot plasma are different, and both energy increase rates are determined primary by the magnetic field strengths.
Spectral Cross-Calibration of the Konus-Wind, the Suzaku/WAM, and the Swift/BAT Data Using Gamma-Ray Bursts
Authors: Sakamoto Takanori , Pal'SHIN Valentin , Yamaoka Kazutaka , Ohno Masanori , Sato Goro , Aptekar Rafail , Barthelmy Scott D. , Baumgartner Wayne H. , Cummings Jay R. , Fenimore Edward E. , Frederiks Dmitry , Gehrels Neil , Golenetskii Sergey , Krimm Hans A. , Markwardt Craig B. , Onda Kaori , Palmer David M. , Parsons Ann M. , Stamatikos Michael , Sugita Satoshi , Tashiro Makoto , Tueller Jack , Ukwatta Tilan N. 
Published: March 2014

Abstract
We report on the spectral cross-calibration results of the Konus-Wind, the Suzaku/WAM, and the Swift/BAT instruments using simultaneously observed gamma-ray bursts (GRBs). This is the first attempt to use simultaneously observed GRBs as a spectral calibration source to understand systematic problems among the instruments. Based on these joint spectral fits, we find that (1) although a constant factor (a normalization factor) agrees within 20% among the instruments, the BAT constant factor shows a systematically smaller value by 10%–20% compared to that of Konus-Wind, (2) there is a systematic trend that the low-energy photon index becomes steeper by 0.1–0.2 and $E_{\rm peak}$ becomes systematically higher by 10%–20% when including the BAT data in the joint fits, and (3) the high-energy photon index agrees within 0.2 among the instruments. Our results show that cross-calibration based on joint spectral analysis is an important step to understanding the instrumental effects that could be affecting the scientific results from the GRB prompt emission data.
Near- and Mid-Infrared Imaging Study of Young Stellar Objects around LkHα 234
Authors: Kato Eri , Fukagawa Misato , Perrin Marshall D. , Shibai Hiroshi , Itoh Yusuke , Ootsubo Takafumi 
Published: March 2014

Abstract
We present high-resolution (0$''\!\!\!.$2) near-infrared images of the area surrounding the Herbig Be star LkH$\alpha $ 234 taken with the Coronagraphic Imager with Adaptive Optics (CIAO) and the adaptive optics on the Subaru Telescope. The near-infrared ($J$, $H$, $K$, $L'$, and $M'$ bands) images reveal circumstellar structures around LkH$\alpha $ 234 in detail. Eight young stellar object (YSO) candidates (Object B, C, D, E, F, G, NW1, and NW2) were detected at 2$\arcsec$–11$\arcsec$ from LkH$\alpha $ 234. Objects B and C are likely variable stars, which is consistent with a young evolutionary status. Three objects (LkH$\alpha $ 234, NW1, and NW2) were identified in the 11.8$\ \mu$m (SiC) and 17.65$\ \mu$m images obtained with the Long Wavelength Spectrometer (LWS) on the Keck Telescope. NW1 and NW2 are thought to be embedded young stars. We suggest that NW1, and not LkH$\alpha $ 234, is the source illuminating the reflection nebula west of LkH$\alpha $ 234, although Object G may be another candidate. In our images, these objects are located at the center of the 2$\ \mu$m polarization, and NW1 resides at the center of a monopolar cavity. The SED of NW1 suggests that it is a YSO with a spectral type of B6–B7. Object F and G were discovered by our observations at 1$''\!\!\!.$9 and 2$''\!\!\!.$3, respectively, from LkH$\alpha $ 234, and their proximity to LkH$\alpha $ 234 suggests that they may be its lower-mass companions.
Infrared Search for Young Brown Dwarf Companions around Young Stellar Objects in the ρ Ophiuchi and the Serpens Molecular Clouds
Authors: Shirono Chiaki , Itoh Yoichi , Oasa Yumiko 
Published: March 2014

Abstract
We conducted an infrared search for faint companions around 351 young stellar objects in the $\rho$ Ophiuchi molecular cloud and the Serpens molecular cloud. Nine objects in the Spitzer/IRAC archival images were identified as being young stellar companion candidates. They showed an intrinsic infrared excess; one object was extremely red both in the [3.6]$-$[4.5] color and in the [4.5]$-$[5.8] color, and two objects were red in the [4.5]$-$[5.8] color. They were as faint as 15 mag in the [3.6] band. Follow-up $K$-band spectroscopy revealed that the three objects had deep water absorption bands, indicative of low effective temperatures. By comparing their spectra and infrared spectral energy distributions with synthesized spectra of low-temperature objects, we derived the effective temperatures and continuum excesses for these objects. It is very likely that one is a low-mass stellar companion, and two others are young brown dwarf companions associated with young stellar objects.
Detection of Phosphorus Nitride in the Lynds 1157 B1 Shocked Region
Authors: Yamaguchi Takahiro , Takano Shuro , Sakai Nami , Sakai Takeshi , Liu Sheng-Yuan , Su Yu-Nung , Hirano Naomi , Takakuwa Shigehisa , Aikawa Yuri , Nomura Hideko , Yamamoto Satoshi 
Published: March 2014

Abstract
We have observed the $J$$=$ 2–1 rotational emission line of PN toward the low-mass star forming region L 1157 with the Nobeyama 45 m telescope. The PN line has been detected toward the two shocked regions (B1 and B2) caused by the interaction between the blue lobe of the outflow from the protostar IRAS 20386$+$6751 and the ambient gas, whereas it has not been detected toward the protostar position. The fractional abundances of PN relative to H$_2$ are evaluated to be (2–6) $\times$ 10$^{-10}$ and (3–7) $\times$ 10$^{-10}$ toward B1 and B2, respectively. Detection of PN in the B1 and B2 positions indicates that the formation of PN can be triggered by shocks. It seems most likely that PN is formed in the gas phase from PH$_3$ evaporated from grain mantles, as suggested by the existing chemical model.
Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. III. The Third Year (2010–2011)
Authors: Kato Taichi , Maehara Hiroyuki , Miller Ian , Ohshima Tomohito , de Miguel Enrique , Tanabe Kenji , Imamura Kazuyoshi , Akazawa Hidehiko , Kunitomi Nanae , Takagi Ryosuke , Nose Mikiha , Hambsch Franz-Josef , Kiyota Seiichiro , Pavlenko Elena P. , Baklanov Aleksei V. , Antonyuk Oksana I. , Samsonov Denis , Sosnovskij Aleksei , Antonyuk Kirill , Andreev Maksim V. , Morelle Etienne , Dubovsky Pavol A. , Kudzej Igor , Oksanen Arto , Masi Gianluca , Krajci Thomas , Pickard Roger D. , Sabo Richard , Itoh Hiroshi , Stein William , Dvorak Shawn , Henden Arne , Nakagawa Shinichi , Noguchi Ryo , Iino Eriko , Matsumoto Katsura , Nishitani Hiroki , Aoki Tomoya , Kobayashi Hiroshi , Akasaka Chihiro , Bolt Greg , Shears Jeremy , Ruiz Javier , Shugarov Sergey Yu. , Chochol Drahomir , Parakhin Nikolai A. , Monard Berto , Shiokawa Kazuhiko , Kasai Kiyoshi , Staels Bart , Miyashita Atsushi , Starkey Donn R. , Ögmen Yenal , Littlefield Colin , Katysheva Natalia , Sergey Ivan M. , Denisenko Denis , Tordai Tamas , Fidrich Robert , Goranskij Vitaly P. , Virtanen Jani , Crawford Tim , Pietz Jochen , Koff Robert A. , Boyd David , Brady Steve , James Nick , Goff William N. , Itagaki Koh-ichi , Nishimura Hideo , Nakashima Youichirou , Yoshida Seiichi , Stubbings Rod , Poyner Gary , Maeda Yutaka , Korotkiy Stanislav A. , Sokolovsky Kirill V. , Ueda Seiji 
Published: March 2014

Abstract
Continuing the project described by Kato et al. (2009, PASJ, 61, S395), we collected the times of superhump maxima for 51 SU UMa-type dwarf novae, mainly observed during the 2010–2011 season. Although most of the new data for systems with short superhump periods basically confirmed the findings by Kato et al. (ibid.) and Kato et al. (2010, PASJ, 62, 1525), the long-period system GX Cas showed an exceptionally large positive-period derivative. An analysis of public Kepler data of V344 Lyr and V1504 Cyg yielded less-striking stage transitions. In V344 Lyr, there was a prominent secondary component growing during the late stage of superoutbursts, and this component persisted for at least two more cycles of successive normal outbursts. We also investigated the superoutburst of two conspicuous eclipsing objects: HT Cas and the WZ Sge-type object SDSS J080434.20$+$510349.2. Strong beat phenomena were detected in both objects, and late-stage superhumps in the latter object had an almost constant luminosity during repeated rebrightenings. The WZ Sge-type object SDSS J133941.11$+$484727.5 showed a phase reversal around the rapid fading from the superoutburst. The object showed a prominent beat phenomenon, even after the end of the superoutburst. A pilot study of superhump amplitudes indicated that the amplitude of superhumps is strongly correlated with the orbital period, and the dependence on the inclination is weak in systems with inclinations smaller than 80$^{\circ}$.
A Planetary Companion to the Intermediate-Mass Giant HD 100655
Authors: Omiya Masashi , Han Inwoo , Izumiura Hideyuki , Lee Byeong-Cheol , Sato Bun'ei , Kim Kang-Min , Seog Yoon Tae , Kambe Eiji , Yoshida Michitoshi , Masuda Seiji , Toyota Eri , Urakawa Seitaro , Takada-Hidai Masahide 
Published: March 2014

Abstract
A precise radial-velocity survey conducted by a Korean–Japanese planet search program revealed a planetary companion around the intermediate-mass clump giant HD 100655. The radial velocity of the star exhibits a periodic Keplerian variation with a period, semi-amplitude, and eccentricity of 157.57 d, 35.2 m s$^{-1}$, and 0.085, respectively. Adopting an estimated stellar mass of 2.4$\ M_{\odot}$, we confirmed the presence of a planetary companion with a semi-major axis of 0.76 AU and a minimum mass of 1.7$\ M_{\mathrm{J}}$. The planet is the lowest-mass planet yet discovered around clump giants with masses greater than 1.9$\ M_{\odot}$.
Suzaku Investigation into the Nature of the Nearest Ultraluminous X-Ray Source, M33 X-8
Authors: Isobe Naoki , Kubota Aya , Sato Hiroshi , Mizuno Tsunefumi 
Published: March 2014

Abstract
The X-ray spectrum of the nearest ultraluminous X-ray source, M 33 X-8, obtained by Suzaku during 2010 January 11–13, was closely analyzed in order to examine its nature. It is, by far, the only data with the highest signal statistic in the 0.4–10 keV range. Despite being able to reproduce the X-ray spectrum, Comptonization of the disk photons failed to give a physically meaningful solution. A modified version of the multi-color disk model, in which the dependence of the disk temperature on the radius is described as $ r^{-p}$ , with $ p$ being a free parameter, can also approximate the spectrum. From this model, the innermost disk temperature and bolometric luminosity were obtained as $ T_{\rm in}$$ =$ 2.00$ _{-0.05}^{+0.06}$ keV and $ L_{\rm disk}$$ =$ 1.36 $ \times$ 10$ ^{39}$ (cos $ i$ )$ ^{-1}$ erg s$ ^{-1}$ , respectively, where $ i$ is the disk inclination. A small temperature gradient of $ p$$ =$ 0.535$ _-0.005^{+0.004}$ , together with the high disk temperature, is regarded as signatures of the slim accretion disk model, suggesting that M 33 X-8 was accreting at a high mass-accretion rate. With a correction factor for the slim-disk taken into account, the innermost disk radius, $ R_{\rm in}$$ =$ 81.9$ _-6.5^{+5.9}$ (cos$ i$ )$ ^{-0.5}$ km, corresponds to a black-hole mass of $ M$$ \sim$ 10 $ M_{\odot}$ (cos $ i$ )$ ^{-0.5}$ . Accordingly, the bolometric disk luminosity is estimated to be about 80(cos $ i$ )$ ^{-0.5}$ % of the Eddington limit. A numerically calculated slim-disk spectrum was found to reach a similar result. Thus, the extremely super-Eddington luminosity is not required to explain the nature of M 33 X-8. This conclusion is utilized to argue for the existence of intermediate-mass black holes with $ M$$ \gtrsim$ 100$ M_{\odot}$ radiating at the sub/trans-Eddington luminosity, among ultraluminous X-ray sources with $ L_{\rm disk}$$ \gtrsim$ 10$ ^{40}$ erg s$ ^{-1}$ .