bluuebunny/crossref_metadata_2025_split huggingface dataset:
Simulation of the EUV Spectrum of Ca XVI
Authors: Liang Ya Qiong , Liu Hong , Zhong Jia Yong 
Published: March 2014

Abstract
The extreme ultraviolet (EUV) spectrum of a Boron-like Ca ion was simulated by using a relativistic multi-configuration atomic package. As compared to previous work [Keenan et al.(1998)], the present study involved indirect processes, such as collision ionization, radiative recombination, dielectronic recombination, and resonance excitation from or to Beryllium-like and Carbon-like Ca ions. The effects of these processes were using three models, named one-, two-, and three-ion. We have found that these indirect processes are important to simulate the EUV spectrum of the Boron-like Ca ion, which will affect the diagnostics of astronomical and laboratory plasmas.
Astrometry of H2O Masers in Nearby Star-Forming Regions with VERA II SVS 13 in NGC 1333
Authors: Hirota Tomoya , Bushimata Takeshi , Choi Yoon Kyung , Honma Mareki , Imai Hiroshi , Iwadate Kenzaburo , Jike Takaaki , Kameya Osamu , Kamohara Ryuichi , Kan-Ya Yukitoshi , Kawaguchi Noriyuki , Kijima Masachika , Kobayashi Hideyuki , Kuji Seisuke , Kurayama Tomoharu , Manabe Seiji , Miyaji Takeshi , Nagayama Takumi , Nakagawa Akiharu , Oh Chung Sik , Omodaka Toshihiro , Oyama Tomoaki , Sakai Satoshi , Sasao Tetsuo , Sato Katsuhisa , Shibata Katsunori M. , Tamura Yoshiaki , Yamashita Kazuyoshi 
Published: March 2014

Abstract
We report on the results of multiepoch very long baseline interferometry (VLBI) observations with VERA (VLBI Exploration of Radio Astrometry) of the 22 GHz H$_{2}$O masers associated with the young stellar object SVS 13 in the NGC 1333 region. We carried out phase-referencing VLBI astrometry, and measured the annual parallax of the maser features in SVS 13 of 4.25$\pm$0.32mas, corresponding to a distance of 235$\pm$18pc from the Sun. Our result is consistent with a photometric distance of 220 pc, previously reported. Even though the maser features were detectable only for 6 months, the present result provides the distance to NGC 1333 with much higher accuracy than photometric methods. The absolute positions and proper motions have been derived, revealing that the H$_{2}$O masers with LSR (local standard of rest) velocities of 7–8kms$^{-1}$ are most likely associated with VLA4A, which is a radio counterpart of SVS 13. It is currently difficult to attribute the observed proper motions of the maser features to either the jet or the rotating circumstellar disk associated with VLA4A, which should be investigated through future high-resolution astrometric observations of VLA4A and other radio sources in NGC 1333.
Shock Waves and Line-Profile Variation in roAp Stars
Authors: Shibahashi Hiromoto , Gough Douglas , Kurtz Donald W. , Kambe Eiji 
Published: March 2014

Abstract
Line-profile variation of NdIII and PrIII spectrum lines of roAp stars obtained with high spectral resolution and high time resolution seem to be similar to those seen in rapidly rotating B-type line-profile variables: features in the lines appear to move smoothly from blue to red, but return to the blue discontinuously. It has been argued in the past that such behaviour is in disagreement with the oblique-pulsator interpretion of the photometric observations. We point out why that argument is invalid. We propose that the properties of the observed line-profile variation can in principle be explained as a manifestation of a shocked wave train propagating upwards through an acoustically thick layer high in the atmosphere, and demonstrate that it is consistent with the underlying pulsation being an axisymmetric low-degree, probably dipole oscillation more-or-less aligned with the magnetic axis, in accord with the oblique-pulsator model.
Hot and Cool Plasmoid Ejections Associated with a Solar Flare
Authors: Ohyama Masamitsu , Shibata Kazunari 
Published: March 2014

Abstract
A 1993 May 14 flare was associated with both X-ray plasma ejection as hot plasmoid ejection and H$\alpha$ filament eruption as cool plasma ejection. The flare proceeded through two stages according to a GOES soft X-ray observation. In the first stage, an X-ray plasma ejection, an H$\alpha$ filament eruption, and a chain of pointlike H$\alpha$ brightenings occurred. In the second stage, an H$\alpha$ two-ribbon flare and an X-ray arcade structure were seen in H$\alpha$ and soft X-ray images, respectively. The X-ray plasmoid and the eruptive H$\alpha$ filament were in the same current sheet. The X-ray plasmoid started to rise with a speed of $\sim$270kms$^{-1}$ temporally after the H$\alpha$ filament eruption. The top part of the X-ray plasmoid moved together with the eruptive filament. They were then decelerated before the main peak of the hard X-ray emission. The X-ray plasmoid was not a bloblike feature, as the eruptive H$\alpha$ filament, but a loop structure. Our results indicate that the X-ray plasmoid was not the heated part of the H$\alpha$ filament.
Central Spiral Structure of Molecular Gas in Maffei 2
Authors: Kuno Nario , Nakanishi Kouichiro , Sorai Kazuo , Shibatsuka Toshihito 
Published: March 2014

Abstract
The distribution and kinematics of molecular gas in the central region of the barred spiral galaxy Maffei 2 were investigated using a data set of $^{12}$ CO(1-0), $^{12}$ CO(2–1), CS(2–1) lines, and 103 GHz continuum. We found that the offset ridges along the kpc-scale bar continue to the central spiral structure embedded in a weak oval structure, which is regarded as an $x$ 2 orbit in the bar potential. The spiral structure continues toward the center, diverging from the oval structure. The size of these structures is less than $R$$\sim$ 100 pc. The mass concentration within $R =$ 35 pc is estimated to be $2 \times 10^{8} M_{\odot}$ . The high mass concentration is consistent with theoretical predictions concerning the creation of such a nuclear spiral structure. A comparison with tracers of dense gas and star-forming region suggests that the dense molecular gas traced by the CS(2–1) line is formed at the crossing points of the $x$ 1 and $x$ 2 orbits and the star-forming region appears after $2 \times 10^{5}$ yr, which is comparable to the free-fall time of dense gas traced by the CS line ( $\sim$$10^{5}$ cm $^{-3}$ ).
Heavy Element Analysis of X-Ray Faint Elliptical Galaxies
Authors: Tozuka Miyako , Fukazawa Yasushi 
Published: March 2014

Abstract
Past ASCA and ROSAT observations could not support the general view that elliptical galaxies are sources of metals in the intracluster medium, since observational results have shown that X-ray faint elliptical galaxies exhibit too low metal abundances of hot interstellar medium (ISM). We investigated the radial profiles of the temperature and abundance of 9 X-ray faint elliptical galaxies using the Chandra data. It is found that the heavy element abundance is as high as $\sim$0.7 solar at the central region. Moreover, toward the periphery of galaxies, the metallicity sharply declines. Therefore, the existence of low-metallicity intergalactic gas around X-ray faint elliptical galaxies is indicated. We also investigated the abundance ratios among several elements of 5 X-ray faint elliptical galaxies using the XMM-Newton data, and obtained a hint that the O$/$Fe ratio of X-ray faint elliptical galaxies is smaller than that of X-ray bright elliptical galaxies. This result perhaps indicates that, in X-ray faint elliptical galaxies, the contribution of SNeIa is smaller than that in X-ray bright ones, and it is speculated that many of the metals in ISM of X-ray faint elliptical galaxies have escaped into the surrounding space.
Milne–Eddington Solutions for Relativistic Plane-Parallel
Flows
Authors: Fukue Jun 
Published: March 2014

Abstract
Radiative transfer in a relativistic plane-parallel flow, e.g., an accretion-disk wind, has been examined using a fully special-relativistic treatment. Under the assumption of a constant flow speed, for a relativistically moving atmosphere, we analytically obtained generalized Milne–Eddington solutions of radiative moment equations: the radiation energy density, the radiative flux, and the radiation pressure. In the static limit these solutions reduce to the traditional Milne–Eddington ones for a plane-parallel static atmosphere, whereas the source function nearly becomes constant as the flow speed increases. Using the analytical solutions, we analytically integrated the relativistic transfer equation to obtain the specific intensity. This specific intensity also reduces to the Milne–Eddington case in the static limit, while the emergent intensity is strongly enhanced toward the flow direction due to Doppler and aberration effects as the flow speed increases (relativistic peaking).
Aligned Molecular Clouds towards SS 433 and L = 348${\rlap{\hskip.75pt{^\circ}}\hskip.75pt.\hskip1pt}$5: Possible Evidence for a Galactic “Vapor Trail” Created by a Relativistic Jet
Authors: Yamamoto Hiroaki , Ito Shingo , Ishigami Shinji , Fujishita Motosuji , Kawase Tokuichi , Kawamura Akiko , Mizuno Norikazu , Onishi Toshikazu , Mizuno Akira , Clure-Griffiths McNaomi M. , Fukui Yasuo 
Published: March 2014

Abstract
We carried out a detailed analysis of the NANTEN $^{12}$CO ($J=$ 1–0) dataset in two large areas towards SS 433 ($l \sim$ 40$^\circ$) and $l \sim$ 348${\rlap{\hskip.75pt{^\circ}}\hskip.75pt.\hskip1pt}$5. In SS 433, we detected ten clouds, which are well aligned nearly along the axis of an X-ray jet emanating from SS 433 at $V_{\rm LSR}$ = 42–56 km s$^{-1}$. The total length of the feature is $\sim\;$300 pc, three-times longer than that of the X-ray jet, at 3 kpc. Towards $l \sim$348${\rlap{\hskip.75pt{^\circ}}\hskip.75pt.\hskip1pt}$5, we detected four aligned clouds at $V_{\rm LSR}$ = $-$80–$-$100 km s$^{-1}$, nearly perpendicular to the Galactic plane. The total length of the feature is $\sim\;$400 pc at 6 kpc. In both cases, the CO clouds are distributed at $\mid{b}\mid\;\sim$ 1${}^\circ$–5${}^\circ$ and their alignments and coincidence in velocity should be rare, suggesting that they are physically associated. We present a scenario to explain these aligned clouds in which the interaction between a relativistic jet and the interstellar medium induced molecular cloud formation over the last $\sim\;$10$^{5\hbox{--}6}$yr. It is suggested that the timescale of the relativistic jet may be considerably larger, on the order of 10$^{5\hbox{--}6}$yr, than previously thought in SS 433. The driving engine of the jet is obviously SS 433, itself, in SS 433, although the engine is not yet identified in $l \sim$348${\rlap{\hskip.75pt{^\circ}}\hskip.75pt.\hskip1pt}$5 among possible several candidates detected in X-rays and TeV gamma rays.
Vertical Temperature Structures of the Solar Corona Derived with the Hinode X-Ray Telescope
Authors: Kano Ryouhei , Sakao Taro , Narukage Noriyuki , Tsuneta Saku , Kotoku Jun’ichi , Bando Takamasa , Edward DeLuca , Lundquist Loraine , Golub Leon , Hara Hirohisa , Matsuzaki Keiichi , Shimojo Masumi , Shibasaki Kiyoto , Shimizu Toshifumi , Nakatani Ichiro 
Published: March 2014

Abstract
We obtained temperature structures in faint coronal features above and near the solar limb with the X-Ray Telescope aboard the Hinode satellite by accurately correcting the scattered X-rays from surrounding bright regions with occulted images during the solar eclipses. Our analysis yields a polar coronal hole temperature of about 1.0 MK and an emission measure in the range of 10$^{25.5}$–10$^{26.0}$cm$^{-5}$. In addition, our methods allow us to measure the temperature and emission measure of two distinct quiet-Sun structures: radial (plume-like) structures near the boundary of the coronal-hole and diffuse quiet Sun regions at mid-latitudes. The radial structures appear to have increasing temperature with height during the first 100 Mm, and constant temperatures above 100 Mm. For the diffuse quiet-Sun region the temperatures are the highest just above the limb, and appear to decrease with height. These differences may be due to different magnetic configurations.
A Bipolar Outflow of the M-Type Giant IRC −10414 Traced by HO Maser Emission
Authors: Maeda Toshihisa , Imai Hiroshi , Omodaka Toshihiro , Kobayashi Hideyuki , Shibata Katsunori M. , Bushimata Takeshi , Choi Yoon Kyung , Hirota Tomoya , Honma Mareki , Horiai Koji , Inomata Noritomo , Iwadate Kenzaburo , Jike Takaaki , Kameno Seiji , Kameya Osamu , Kamohara Ryuichi , Kan-ya Yukitoshi , Kawaguchi Noriyuki , Kuji Seisuke , Kurayama Tomoharu , Manabe Seiji , Miyaji Takeshi , Nagayama Takumi , Nakagawa Akiharu , Nakashima Kouichiro , Oh Chung Sik , Oyama Tomoaki , Sakai Satoshi , Sakakibara Seiichiro , Sato Katsuhisa , Shimizu Rie , Shintani Motonobu , Sora Kasumi , Suda Hiroshi , Tamura Yoshiaki , Yamashita Kazuyoshi 
Published: March 2014

Abstract
We report on results of five-epoch VLBI observations of H$_{2}$O maser emission in the M-type star IRC $-$10414, carried out with the VLBI Exploration of Radio Astrometry (VERA). The maser distribution extends over an area of 70mas$\times$260mas and exhibits a bipolar structure. The relative proper motions of 17 maser features were measured during the monitoring observations spanning nine months. The distance to IRC $-$10414 was re-estimated on the basis of the statistical treatment of parallax and the model-fitting method, yielding $D=$ 3.1$\pm$0.4kpc and $D=$ 2.0$\pm$0.2kpc, respectively. The estimated distance, $D=$ 2-3kpc, is much larger than that previously adopted. The stellar luminosity of IRC $-$10414 is also re-estimated to be $L_{\ast}\sim 9\times10^{4}$($D/$2kpc)$^{2} L_{\odot}$, much brighter by a factor of 10-20 than previously adopted ($L_{\ast} \sim 10000L_{\odot}$). The maser motions exhibit not only a spherically expanding flow with a velocity of $\sim$ 10($D/$2kpc)kms$^{-1}$, but also a faster bipolar outflow with a major axis in the north-south direction and at a small inclination angle with respect to the celestial sphere. These characteristics of the star and the circumstellar envelope seen in IRC $-$10414 are very similar to those in some supergiants exhibiting bipolar stellar mass loss.
The 2006 November Outburst of EG Aquarii: the SU UMa Nature Revealed
Authors: Imada Akira , Stubbings Rod , Kato Taichi , Uemura Makoto , Krajci Thomas , Torii Ken’ichi , Sugiyasu Kei , Kubota Kaori , Moritani Yuuki , Ishioka Ryoko , Masi Gianluca , Kiyota Seiichiro , Monard L. A. G. , Maehara Hiroyuki , Nakajima Kazuhiro , Arai Akira , Ohsugi Takashi , Yamashita Takuya , Kawabata Koji S. , Nagae Osamu , Chiyonobu Shingo , Fukazawa Yasushi , Mizuno Tsunefumi , Katagiri Hideaki , Takahashi Hiromitsu , Ueda Atsushi , Hayashi Takehiro , Okita Kiichi , Yoshida Michitoshi , Yanagisawa Kenshi , Sato Shuji , Kino Masaru , Kitagawa Masahiro , Sadakane Kozo , Nogami Daisaku 
Published: March 2014

Abstract
We report on time-resolved CCD photometry of the cataclysmic variable EG Aquarii during a 2006 November outburst. During the outburst, superhumps were unambiguously detected with a mean period of 0.078828(6) d, allowing for the first time to classify the object as an SU UMa-type dwarf nova. It also turned out that the outburst contained a precursor. At the end of the precursor, immature profiles of humps were observed. By a phase analysis of these humps, we interpreted the features as being superhumps. This is the second example that the superhumps were shown during a precursor. Near the maximum stage of the outburst, we discovered an abrupt shift of the superhump period by ${\sim\;}$0.002 d. After the supermaximum, the superhump period decreased at a rate of $\dot{P}/P =$$-$8.2${\;\times\;}$10$^{-5}$, which is typical for SU UMa-type dwarf novae. Although the outburst light curve was characteristic of SU UMa-type dwarf novae, long-term monitoring of the variable shows no outbursts over the past decade. We also comment on the basic properties of long period and inactive SU UMa-type dwarf novae.
Integral and RXTE/ASM Observations on IGR J17098−3628
Authors: Chen Yu-Peng , Zhang Shu , Schurch Nick , Wang Jian-Min , Collmar Werner , Li Ti-Pei , Qu Jin-Lu , Zhang Cheng-Min 
Published: March 2014

Abstract
To further probe the possible nature of the unidentified source IGR J17098$-$3628, we have carried out a detailed analysis of its long-term time variability, as monitored by Rossi X-ray Timing Explorer/All Sky Monitor (RXTE/ASM), and of its hard X-ray properties, as observed by the International Gamma-Ray Astrophysics Laboratory (INTEGRAL). INTEGRAL has monitored this sky region for years, and significantly detected IGR J17098$-$3628 only when the source was in its dubbed active state. In particular, at $\ge$20 keV, Imager on Board of the INTEGRAL Satellite/INTEGRAL Soft Gamma-Ray Imager (IBIS/ISGRI) caught an outburst in 2005 March, lasting for $\sim$5 d with a detection significance of 73$\sigma$ (20-40 keV) and with emission at $/lt$200 keV. ASM observations have revealed that the outburst of the soft X-ray lightcurve is similar to that detected by INTEGRAL; however the peak of the soft X-ray lightcurve lags behind, or is preceded by, the hard X-ray ($/gt$20 keV) outburst by $\sim$2 d. This resembles the behavior of X-ray novae like XN 1124$-$683, and hence further suggests a Low-Mass X-ray Binary (LMXB) nature for IGR J17098$-$3628. While the quality of the ASM data prevents us from drawing any definite conclusions, these discoveries are important clues that, coupled with future observations, will help us to resolve the nature of IGR J17098$-$3628 that is unknown so far.
Dual-Beam Delay Calibration for VERA
Authors: Honma Mareki , Kijima Masachika , Suda Hiroshi , Kawaguchi Noriyuki , Kobayashi Hideyuki , Bushimata Takeshi , Shimizu Rie , Yoshimura Akane , Sasao Tetsuo , Hirota Tomoya , Imai Hiroshi , Iwadate Kenzaburo , Jike Takaaki , Kameya Osamu , Kamohara Ryuichi , Kuji Seisuke , Kurayama Tomoharu , Manabe Seiji , Miyaji Takeshi , Nakagawa Akiharu , Omodaka Toshihiro , Oyama Tomoaki , Sakai Satoshi , Sato Katsuhisa , Shibata Katsunori M. , Tamura Yoshiaki 
Published: March 2014

Abstract
We present the technique of instrumental delay calibration for the dual-beam system of VLBI Exploration of Radio Astrometry (VERA), namely, the horn-on-dish method, in which artificial noise sources are mounted on the antenna feedome base and a wide-band radio noise is injected into the dual-beam receivers after reflection by a subreflector. We introduce the basic concept of calibration with the horn-on-dish method, and also present results of the experiments to evaluate its calibration accuracy. Detailed comparisons between model path calculations and measured paths from the noise sources show that the horn-on-dish method can calibrate the dual-beam delay difference in the antenna structure and receiver within an $\sim$0.1mm level. We estimated that the systematic error in the calibration does not exceed 0.127mm, which was evaluated at an elevation angle of 15$^\circ$. This error corresponds to an astrometric error of $\sim$11$\mu$as with VERA's maximum baseline. An experimental confirmation of the systematic error in the horn-on-dish method has also been obtained by using a pair of 10m and VERA's 20m antennas at the Mizusawa station, demonstrating that the systematic difference between the dual-beam delay difference measured with noise sources and that for celestial objects was 0.118mm, being consistent with the above estimate.
Distance to NGC 281 in a Galactic Fragmenting Superbubble: Parallax Measurements with VERA
Authors: Sato Mayumi , Hirota Tomoya , Honma Mareki , Kobayashi Hideyuki , Sasao Tetsuo , Bushimata Takeshi , Choi Yoon Kyung , Imai Hiroshi , Iwadate Kenzaburo , Jike Takaaki , Kameno Seiji , Kameya Osamu , Kamohara Ryuichi , Kan-Ya Yukitoshi , Kawaguchi Noriyuki , Kim Mi Kyoung , Kuji Seisuke , Kurayama Tomoharu , Manabe Seiji , Matsui Makoto , Matsumoto Naoko , Miyaji Takeshi , Nagayama Takumi , Nakagawa Akiharu , Nakamura Kayoko , Oh Chung Sik , Omodaka Toshihiro , Oyama Tomoaki , Sakai Satoshi , Sato Katsuhisa , Shibata Katsunori M. , Tamura Yoshiaki , Yamashita Kazuyoshi 
Published: March 2014

Abstract
We have used the Japanese VLBI array VERA to perform high-precision astrometry of an H$_2$O maser source in the Galactic star-forming region NGC 281 West, which has been considered to be part of a 300-pc superbubble. We successfully detected a trigonometric parallax of 0.355$\pm$0.030mas, corresponding to a source distance of 2.82$\pm$0.24kpc. Our direct distance determination of NGC 281 has resolved a large distance discrepancy between previous photometric and kinematic studies; likely NGC 281 is in the far side of the Perseus spiral arm. The source distance as well as the absolute proper motions were used to demonstrate the 3D structure and expansion of the NGC 281 superbubble, $\sim\;$650pc in size parallel to the Galactic disk and with a shape slightly elongated along the disk or spherical, but not vertically elongated, indicating that the superbubble expansion may be confined to the disk. We estimate the expansion velocity of the superbubble as being $\sim\;20$km s$^{-1}$, both perpendicular to and parallel to the Galactic disk with a consistent timescale of $\sim\;20$Myr.
SiO Maser Observations toward Orion-KL with VERA
Authors: Kim Mi Kyoung , Hirota Tomoya , Honma Mareki , Kobayashi Hideyuki , Bushimata Takeshi , Choi Yoon Kyung , Imai Hiroshi , Iwadate Kenzaburo , Jike Takaaki , Kameno Seiji , Kameya Osamu , Kamohara Ryuichi , Kan-Ya Yukitoshi , Kawaguchi Noriyuki , Kuji Seisuke , Kurayama Tomoharu , Manabe Seiji , Matsui Makoto , Matsumoto Naoko , Miyaji Takeshi , Nagayama Takumi , Nakagawa Akiharu , Oh Chung Sik , Omodaka Toshihiro , Oyama Tomoaki , Sakai Satoshi , Sasao Tetsuo , Sato Katsuhisa , Sato Mayumi , Shibata Katsunori M. , Tamura Yoshiaki , Yamashita Kazuyoshi 
Published: March 2014

Abstract
We present results of phase-referencing VLBI observations of SiO masers in the Orion-KL region made with VERA. Using a strong maser spot in the 43GHz $v =$ 2 $J=$ 1-0 emission, we derived the trigonometric parallax of Orion-KL to be 2.39$\pm$0.03mas, corresponding to a distance of 418$\pm$6pc, with the highest accuracy among existing parallax measurements of the source. We made a superimposed image of $v =$ 1 $J=$ 1-0 and $v =$ 2 $J=$ 1-0 maser features in Orion-KL based on absolute positions obtained from the phase-referencing astrometry with a common reference source. The maser features of both transitions show similar X-shaped distributions centered at Source I. However, in each of the four arms of the X-shape, the SiO $v =$ 2 features tend to lie closer to Source I than the SiO $v =$ 1 features. The radial velocities of the maser emission decrease with the distance from Source I. The spatial and radial velocity distributions of the SiO masers suggest that the SiO masers lie in the rotating materials associated with a disk around Source I, rather than a decelerating outflow.
Asymmetric Ejecta Distribution of the Cygnus Loop Revealed with Suzaku
Authors: Katsuda Satoru , Tsunemi Hiroshi , Miyata Emi , Mori Koji , Namiki Masaaki , Nemes Norbert , Miller Eric D. 
Published: March 2014

Abstract
We observed a linearly sliced area of the Cygnus Loop from the north-east to the south-west with Suzaku in seven pointings. After dividing the entire fields of view (FOV) into 119 cells, we extracted spectra from all of the cells and performed spectral analysis for them. We then applied both one- and two-component non-equilibrium ionization (NEI) models for all of the spectra, finding that almost all were significantly better fitted by the two-component NEI model rather than the one-component NEI model. Judging from the abundances, the high-$kT_\mathrm{e}$ component must be the ejecta component, while the low-$kT_\mathrm{e}$ component comes from the swept-up matter. Therefore, the ejecta turn out to be distributed inside a large area (at least our FOV) of the Cygnus Loop. We divided the entire FOV into northern and southern parts, and found that the ejecta distributions were asymmetric to the geometric center: the ejecta of Si, S, and Fe seem to be distributed more in the south than in the north of the Cygnus Loop by a factor of $\sim$2. The degree of ejecta-asymmetry is consistent with that expected by recent supernova explosion models.