bluuebunny/crossref_metadata_2025_split huggingface dataset:
Large-Field CO (J = 1→0) Observations of the Starburst Galaxy M 82
Authors: Salak Dragan , Nakai Naomasa , Miyamoto Yusuke , Yamauchi Aya , Tsuru Takeshi G. 
Published: March 2014

Abstract
We present large-field (15.7 $ \times$ 16.9 arcmin$ ^2$ ) CO ($ J$ $ =$ 1$ \rightarrow$ 0) observations of the starburst galaxy M 82, at an angular resolution of 22$ ''$ with the NRO 45-m telescope. The CO emission was detected in the galactic disk, outflow (driven by the galactic wind) up to $ \sim$ 2 kpc above the galactic plane in the halo, and in tidal streams. The kinematics of the outflow (including CO line splitting) suggests that it has the shape of a cylinder that is diverging outwards. The mass and kinetic energy of the molecular gas outflow are estimated to be (0.26–1.0) $ \times$ 10$ ^{9}\ M_{\odot}$ and (1–4) $ \times$ 10$ ^{56}$ erg. A clump of CO gas was discovered 3.5 kpc above the galactic plane; it coincides with a dark lane previously found in X-ray observations, and a peak in H I emission. A comparison with H I, hot molecular hydrogen and dust suggests that the molecular gas shows signatures of warm and cool components in the outflow and tidal streams, respectively.
Universal Scaling Law in Long Gamma-Ray Bursts
Authors: tsutsui Ryo , shigeyama Toshikazu 
Published: March 2014

Abstract
The overwhelming diversity of long gamma-ray bursts (LGRBs), discovered after the launch of the Swift satellite, is a major obstacle to LGRB studies. Recently, it was shown that the prompt emission of LGRBs can be classified into three subclasses: Type I and Type II LGRBs, populating separate fundamental planes in a 3D space defined by the peak luminosity, the duration, and the spectral peak energy, and outliers belonging to none of these planes. Here, we show that Type I LGRBs exhibit different shapes of light curves from that of Type II LGRBs. Furthermore, we demonstrate that this classification has uncovered a new scaling law concerning the light curve of Type II LGRBs, over a span of 8 orders of magnitude ranging from the prompt emission to the late X-ray afterglow one. The scaled light curve has four distinct phases. The first phase has a characteristic time-scale, while the three subsequent phases exhibit power-law behaviors with different exponents. We attempt a new interpretation in terms of the emission from an optically thick fireball propagating in the cricumstellar matter at relativistic speed, and argue that the four observed phases correspond to its hydrodynamical phases. Our classification scheme succeeds in pinning down intrinsic luminosities of Type II LGRBs through the scaling law with a sample of polymorphic GRBs. Further refinements of this scheme and scaling law will make it possible to use a subclass of LGRBs as new standard candles with the same reliability and accuracy as Type Ia supernovae in more distant universe than the light from supernovae can reach.
On the Origin of Orbital Period Change in WY Cancri: A Genuine Angular-Momentum Loss?
Authors: Chen Wen-Cong 
Published: March 2014

Abstract
WY Cnc is a short-period ($ P$$ =$ 0.829 d) eclipsing RS Canum Venaticorum star, and both components are of the late-type stars. Recently, observations provided by photometric observations and light-time minima show that the orbital period of WY Cnc is experiencing a secular decrease at a rate of $ {d}P/{d}t$$ =$$-$ 1.2 $ \times$ 10$ ^{-7}$ d yr$ ^{-1}$ . In this letter, we consider whether the period change of WY Cnc can originate from angular-momentum loss. In calculations, we assumed that this source has a high wind loss rate of $ \sim$ 10$ ^{-10}$$ M_{\odot}$ yr$ ^{-1}$ . To account for the observation, magnetic braking demands a strong surface magnetic field of $ \gtrsim$ 10000 G, like that of Ap/Bp stars. Furthermore, if this source is perhaps surrounded by a circumbinary disk, and 6% of the wind loss feeds the disk, the tidal torque between the disk and the binary can account for the observed angular-momentum loss rate. Such a strong magnetic field, or an extremely high wind input fraction, seems to be highly unlikely.
Stellar Spectral Subclass Classification Based on Locally Linear Embedding
Authors: Yude Bu , Jingchang Pan , Bin Jiang , Peng Wei 
Published: March 2014

Abstract
Locally linear embedding (LLE) is a recently developed dimension reduction technique. In this paper, we describe how we applied LLE to the stellar subclass classification. We found that LLE classifies the objects with different physical characteristics correctly. We then compared the performance of LLE with that of principal component analysis (PCA) in spectral classification, and found that LLE does better than PCA. We tested the robustness of LLE against the changing of signal-to-noise ratios (SNRs), and found that the performance of LLE is affected by two factors: changing of SNRs and the range of SNRs of the spectra data set. We also studied the variation of LLE parameters, and found that the experiment results are affected by the parameter variation, but not sensitive. Finally, using LLE, we located those objects misclassified by the Sloan Digital Sky Survey pipeline, and estimated its accuracy in classifying stellar subclasses.
Superposition of Cyclotron Lines in Accreting X-Ray Pulsars. II. Increasing B-Field
Authors: Nishimura Osamu 
Published: March 2014

Abstract
Cyclotron lines have been modeled by calculating a superposition of a large number of cyclotron line spectra of photons emerging from different heights of line-forming regions illuminated from above (increasing $B$-field), in addition to ones illuminated from below (decreasing $B$-field), as considered in Paper I (Nishimura 2011, ApJ, 730, 106). This simplified model succeeds to reproduce anharmonic ratios of cyclotron line energies (less than harmonic values), correlations between cyclotron line energies and X-ray intensities observed at different pulse phases, using a line-forming region with increasing $B$-field for the main pulses of Her X-1, Cen X-3, and GX 301$-$ 2. It is also able to reproduce the characteristics of the cyclotron lines in several parts of the secondary pulse of Vela X-1, A 0535$+$ 26, whereas in several parts of both the main and secondary pulses of X 0115$+$ 63. In addition, in the phase-resolved spectra of X 0115$+$ 63, the observed ratios of the centroid energy of the second-harmonic line to the fundamental change from $\sim$ 1.6 to $\sim$ 2.2 with the pulse phase. A combination of the increasing and decreasing $B$-field is able to explain this behavior in terms of the idea that a magnetic-field configuration in a line-forming region can switch from decreasing to increasing $B$-field, and vice versa, as a result of a switch of the primary observed pole, from which the flux mainly comes, with the rotation of the neutron star.
OAO/MITSuME Photometry of Dwarf Novae. I. SU Ursae Majoris
Authors: Imada Akira , Izumiura Hideyuki , Kuroda Daisuke , Yanagisawa Kenshi , Omodaka Toshihiro , Miyanoshita Ryo , Kawai Nobuyuki , Nogami Daisaku 
Published: March 2014

Abstract
We report on simultaneous $g', R_{\rm c}$, and $I_{\rm c}$ photometry of SU Ursae Majoris during 2011 December–2012 February using OAO/MITSuME. Our photometry revealed that quiescence is divided into three types based on the magnitude and color. Quiescent light curves showed complicated profiles with various amplitudes and time scales. Although no superoutbursts were observed during our run, five normal outbursts occurred with intervals of 11–21 d. The shapes of the normal outbursts were characteristic of the outside-in type. During the rising phase of a normal outburst, the light curve showed periodic modulations with a period of ${\sim}$ 0.048111(354) d, but the origin of this peirod was unclear. We examined daily averaged color–color diagrams, and found that two cycles exist. This implies that the thermal limit cycle in SU UMa is complicated. We newly discovered that $g' - R_{\rm c}$ becomes red about 3 days prior to an outburst. Although the working mechanism on this reddening is unclear, we propose two possibilities: one is that the inner portion of the accretion disk is filled by matter and obscures the central white dwarf; the other is that the stagnation effect works in the outer region of the accretion disk.
SSS J122221.7–311523: Double Superoutburst in the Best Candidate for a Period Bouncer
Authors: Kato Taichi , Monard Berto , Hambsch Franz-Josef , Kiyota Seiichiro , Maehara Hiroyuki 
Published: March 2014

Abstract
We observed the 2012–2013 superoutburst of the newly identified transient SSS J122221.7–311523, and found that this object showed two successive superoutbursts. Superhumps grew in amplitude during the second superoutburst, and showed a characteristic feature in their period change reflecting the growth of superhumps. Assuming that the periods of the superhumps in the growing stage [0.07721(1) d] and the post-superoutburst stage [0.07673(3) d] represent the dynamical precession rates at the disk radius of the 3:1 resonance and at the disk radius immediately after the superoutburst, respectively, we found that this object has a very small mass ratio of $q = M_2/M_1 \lt 0.05$. The possible orbital period from quiescent data suggests $q = 0.045$, which is the smallest among mass ratios of hydrogen-rich cataclysmic variables. The long orbital period and low $q$ make this object a perfect candidate for a period bouncer. We suggest that the peculiar feature of the double superoutburst is a result of a low $q$, and may be characteristic of period bouncers.
New Method of Estimating Binary's Mass Ratios by Using Superhumps
Authors: Kato Taichi , Osaki Yoji 
Published: March 2014

Abstract
We propose a new dynamical method of estimating binary's mass ratios by using the period of superhumps in SU UMa-type dwarf novae during the growing stage (the stage A superhumps). This method is based on the working hypothesis that the period of superhumps in the growing stage is determined by the dynamical precession rate at the 3W1 resonance radius, and is suggested in our new interpretation of the superhump period evolution during a superoutburst (2013, PASJ, 65, 95). By comparing objects having known mass ratios, we show that our method can provide sufficiently accurate mass ratios comparable to those obtained by eclipse observations in quiescence. One of the advantages of this method is that it requires neither an eclipse nor any experimental calibration. It is particularly suitable for exploring the low mass-ratio end of the evolution of cataclysmic variables, where the secondary is not detectable by conventional methods. Our analysis suggests that previous determinations of the mass ratio by using superhump periods during a superoutburst were systematically underestimated for low mass-ratio systems, and we provided a new calibration. It reveals that most WZSge-type dwarf novae have either secondaries close to the border of the lower main-sequence or brown dwarfs, and most of the objects have not yet reached the evolutionary stage of period bouncers. Our results are not in contradiction with an assumption that an observed minimum period ($\sim 77$ min) of ordinary hydrogen-rich cataclysmic variables is indeed the minimum period. We highlight how important the early observation of stage A superhumps is, and propose an effective future strategy of observation.
Low-Resolution Spectrum of the Extragalactic Background Light with the AKARI InfraRed Camera
Authors: Tsumura Kohji , Matsumoto Toshio , Matsuura Shuji , Sakon Itsuki , Wada Takehiko 
Published: March 2014

Abstract
The Extragalactic Background Light (EBL) as integrated light from outside of our Galaxy includes information about the early universe and the Dark Ages. We analyzed spectral data of the astrophysical diffuse emission obtained with the low-resolution spectroscopy mode on the AKARI Infra-Red Camera (IRC) in the $1.8-5.3 \mu \textrm m $ wavelength region. Although previous EBL observations in this wavelength region were restricted to observations by DIRBE and IRTS, this study adds a new independent result with negligible contamination of Galactic stars owing to higher sensitivity for point sources. Two other major foreground components, zodiacal light (ZL) and diffuse Galactic light (DGL), were subtracted by taking correlations with ZL brightness estimated by the DIRBE ZL model and with the $100 \mu \textrm m $ dust thermal emission, respectively. The isotropic emission was obtained as EBL, which shows significant excess over integrated light of galaxies at $ \lt 4 \mu \textrm m $. The obtained EBL is consistent with the previous measurements by IRTS and DIRBE.
KIC 7524178—an SU UMa-Type Dwarf Nova Predominantly Showing Negative Superhumps throughout Supercycle
Authors: Kato Taichi , Osaki Yoji 
Published: March 2014

Abstract
We analyzed Kepler long-cadence data of KIC 7524178 (= KIS J192254.92+430905.4), and found that it is an SU UMa-type dwarf nova with frequent normal outbursts. The signal of the negative superhump has always been the dominant one, even during the superoutburst, in contrast to our common knowledge about superhumps in dwarf novae. The signal of the positive superhump was only transiently seen during the superoutburst, and it quickly decayed afterward. The frequency variation of the negative superhump was similar to the two previously studied dwarf novae in the Kepler field, V1504 Cyg and V344 Lyr. This is the first object in which the negative superhumps dominate throughout the supercycle. Nevertheless, the superoutburst was faithfully accompanied by the positive superhump, indicating that the tidal eccentric instability is essential for triggering a superoutburst. All the pieces of evidence strengthen the thermal-tidal instability as being the origin of the superoutburst and supercycle, which makes this object the third example in the Kepler field. This object had an unusually small ($\sim 1.0$ mag) outburst amplitude, and we considered that this object has a high mass-transfer rate close to the thermal-stability limit of the accretion disk. The average periods of the negative and positive superhumps, and the candidate period of the orbital motion were 0.07288 d (variable in the range $0.0723–0.0731$ d), 0.0785 d (variable in the range $0.0772–0.0788$ d), and 0.074606(1) d, respectively
Local Enhancement of the Surface Density in the Protoplanetary Ring Surrounding HD 142527
Authors: Fukagawa Misato , Tsukagoshi Takashi , Momose Munetake , Saigo Kazuya , Ohashi Nagayoshi , Kitamura Yoshimi , Inutsuka Shu-ichiro , Muto Takayuki , Nomura Hideko , Takeuchi Taku , Kobayashi Hiroshi , Hanawa Tomoyuki , Akiyama Eiji , Honda Mitsuhiko , Fujiwara Hideaki , Kataoka Akimasa , Takahashi Sanemichi Z. , Shibai Hiroshi 
Published: March 2014

Abstract
We report on ALMA observations of the dust continuum, and $^{13}\textrm {CO} (J=3-2), \textrm {and} \textrm {C}^{18} \textrm{O} (J=3-2)$ line emission toward a gapped protoplanetary disk around HD 142527. The outer horseshoe-shaped disk shows a strong azimuthal asymmetry in the dust continuum with a ratio of $\sim 30$ to 1 at 336 GHz between the northern peak and the southwestern minimum. In addition, the maximum brightness temperature of 24K at its northern area is exceptionally high at 160 au from a star. To evaluate the surface density in this region, the grain temperature needed constraining, and was estimated from the optically thick $^{13}\textrm {CO} (J=3-2)$ emission. The lower limit of the peak surface density was then calculated to be 28 g cm $^{-2}$ by assuming a canonical gas-to-dust mass ratio of 100. This finding implies that the region is locally too massive to withstand self-gravity, since Toomre's $Q \lesssim 1-2$, and thus it may collapse into a gaseous protoplanet. Another possibility is that the gas mass is low enough to be gravitationally stable, and only dust grains are accumulated. In this case, a lower gas-to-dust ratio by at least 1 order of magnitude is required, implying the possible formation of a rocky planetary core.
A Study of Coronal Holes Observed by SOHO/EIT and the Nobeyama Radioheliograph
Authors: Akiyama Sachiko , Gopalswamy Nat , Yashiro Seiji , Mäkelä Pertti 
Published: March 2014

Abstract
Coronal holes (CHs) are areas of reduced emission in EUV and X-ray images that show bright patches of microwave enhancements (MEs) related to magnetic network junctions inside the CHs. A clear correlation between the CH size and the solar wind (SW) speed is well known, but we have less information about the relationship between MEs and other CH and SW properties. We studied the characteristics of 21 equatorial CHs associated with corotating interaction regions (CIRs) during 1996 to 2005. Our CHs were divided into two groups according to the intensity of the associated geomagnetic storms: Dst≤-100 nT (10 events) and &gt; -100 nT (11 events). Using EUV 284 Å images obtained by SOHO/EIT and 17 GHz microwave images obtained by the Nobeyama Radioheliograph (NoRH), we found a linear correlation not only between the maximum SW speed and the area of EUV CH (r = 0.62), but also between the maximum SW speed and the area of the ME (r = 0.79). We also compared the EUVCH areas with and without an overlapping ME. The area of the CHs with an ME is better correlated with the SW speed (r = 0.71) than the area of those without an ME (r = 0.36). Therefore, the radio ME may play an important role in understanding the origin of SW.
Imaging of the Solar Atmosphere by the Siberian Solar Radio Telescope at 5.7 GHz with an Enhanced Dynamic Range
Authors: Kochanov Alexey A. , Anfinogentov Sergey A. , Prosovetsky Dmitry V. , Rudenko George V. , Grechnev Victor V. 
Published: March 2014

Abstract
The Siberian Solar Radio Telescope (SSRT) is a solar-dedicated directly-imaging interferometer observing the Sun at 5.7 GHz. SSRT has operated in the two-dimensional mode since 1996. The imaging principle of SSRT restricts its opportunities in observations of very bright flare sources, while it is possible to use ‘dirty’ images in studies of low-brightness features, which do not overlap with side lobes from bright sources. The interactive CLEAN technique routinely used for SSRT data provides imaging of active regions, but consumes much time and efforts and does not reveal low-brightness features below the CLEAN threshold. The newly developed technique combines the CLEAN routine with the directly-imaging capability of SSRT, and provides clean images with an enhanced dynamic range automatically. These elaborations considerably extend the range of tasks that can be solved with SSRT. We show here some examples of the present opportunities of SSRT, and compare its data with the images produced by the Nobeyama Radioheliograph at 17 GHz as well as observations in different spectral ranges.
Solar Burst Analysis with 3D Loop Models
Authors: Costa Joaquim Eduardo Rezende , de Aguiar SimõES Paulo José , Pinto Tereza Satiko Nishida , Melnikov Victor Fedorovich 
Published: March 2014

Abstract
A sample of Nobeyama flares was selected and analyzed using a loop model for important flare parameters. The model for the flaring region consists of a three-dimensional dipolar magnetic field, and spatial distributions of nonthermal electrons. We constructed a database by calculating the flare microwave emission for a wide range of these parameters. Out of this database with more than 5000 cases, we extracted general flare properties by comparing the observed and calculated microwave spectra. The analysis of the Nobeyama Radio Polarimeter data was mostly based on the center-to-limb variation of the flare properties with looptop and footpoint electron distributions, and for the Nobeyama Radioheliograph maps on the resultant distribution of emission. One important aspect of this work is a comparison of the analysis of a flare using an inhomogeneous source model and a simplistic homogeneous source model. Our results clearly show that the homogeneous source hypothesis is not appropriate to describe the possible flare geometry, and its use can easily produce misleading results in terms of non-thermal electron density and magnetic field strength. A center darkening of flares was also obtained as a geometrical property of the loop-like sources.
Pentavalent Rotavirus Vaccine in Infants With Surgical Gastrointestinal Disease
Authors: McGrath Eric J. , Thomas Ron , Duggan Christopher , Asmar Basim I. 
Published: March 2014

ABSTRACTObjectives:Pentavalent rotavirus vaccine (RV5) has been shown to be well‐tolerated and efficacious in preventing rotavirus gastroenteritis in healthy infants. Safety and immunogenicity of RV5 in infants with surgical gastrointestinal disease have not been studied. The aim of the present study was to evaluate the safety and immunogenicity of RV5 in infants with a history of congenital or acquired intestinal disease requiring resection compared with healthy infants.Methods:Infants with intestinal resection were matched by gestational age and chronological age to healthy infants (controls). Dose 1 of RV5 was given at 10 to 12 weeks of chronological age. Doses 2 and 3 were given at intervals of 4 to 10 weeks, with all 3 doses given by 32 weeks. All infants were monitored for adverse events (AEs) by telephone calls, clinic visits, and parental written reports during the first 42 days after each dose and monthly thereafter by telephone for 12 months. Serum anti‐rotavirus immunoglobulin A (IgA) titers were measured prevaccination and 2 weeks after dose 3.Results:A total of 5 infants with surgical gastrointestinal disease and 3 control subjects were enrolled. All participants (100%) mounted a 3‐fold increase in serum anti‐rotavirus IgA geometric mean titer postvaccination. RV5 administration to surgical infants was well tolerated with a majority of AEs being attributed to the underlying medical condition.Conclusions:Postvaccination serum anti‐rotavirus IgA levels indicate that RV5 is immunogenic in infants with a history of bowel resection, despite varying lengths of residual bowel. RV5 was well tolerated with few vaccine‐related AEs.
Whole‐Exome Sequencing Reveals GPIHBP1 Mutations in Infantile Colitis With Severe Hypertriglyceridemia
Authors: Gonzaga‐Jauregui Claudia , Mir Sabina , Penney Samantha , Jhangiani Shalini , Midgen Craig , Finegold Milton , Muzny Donna M. , Wang Min , Bacino Carlos A. , Gibbs Richard A. , Lupski James R. , Kellermayer Richard , Hanchard Neil A. 
Published: March 2014

ABSTRACTSevere congenital hypertriglyceridemia (HTG) is a rare disorder caused by mutations in genes affecting lipoprotein lipase (LPL) activity. Here we report a 5‐week‐old Hispanic girl with severe HTG (12,031 mg/dL, normal limit 150 mg/dL) who presented with the unusual combination of lower gastrointestinal bleeding and milky plasma. Initial colonoscopy was consistent with colitis, which resolved with reduction of triglycerides. After negative sequencing of the LPL gene, whole‐exome sequencing revealed novel compound heterozygous mutations in GPIHBP1. Our study broadens the phenotype of GPIHBP1‐associated HTG, reinforces the effectiveness of whole‐exome sequencing in Mendelian diagnoses, and implicates triglycerides in gastrointestinal mucosal injury.