bluuebunny/crossref_metadata_2025_split huggingface dataset:
Hard X-Ray Detector (HXD) on Board Suzaku
Authors: Takahashi Tadayuki , Abe Keiichi , Endo Manabu , Endo Yasuhiko , Ezoe Yuuichiro , Fukazawa Yasushi , Hamaya Masahito , Hirakuri Shinya , Hong Soojing , Horii Michihiro , Inoue Hokuto , Isobe Naoki , Itoh Takeshi , Iyomoto Naoko , Kamae Tuneyoshi , Kasama Daisuke , Kataoka Jun , Kato Hiroshi , Kawaharada Madoka , Kawano Naomi , Kawashima Kengo , Kawasoe Satoshi , Kishishita Tetsuichi , Kitaguchi Takao , Kobayashi Yoshihito , Kokubun Motohide , Kotoku Jun’ichi , Kouda Manabu , Kubota Aya , Kuroda Yoshikatsu , Madejski Greg , Makishima Kazuo , Masukawa Kazunori , Matsumoto Yukari , Mitani Takefumi , Miyawaki Ryohei , Mizuno Tsunefumi , Mori Kunishiro , Mori Masanori , Murashima Mio , Murakami Toshio , Nakazawa Kazuhiro , Niko Hisako , Nomachi Masaharu , Okada Yuu , Ohno Masanori , Oonuki Kousuke , Ota Naomi , Ozawa Hideki , Sato Goro , Shinoda Shingo , Sugiho Masahiko , Suzuki Masaya , Taguchi Koji , Takahashi Hiromitsu , Takahashi Isao , Takeda Shin’ichiro , Tamura Ken-ichi , Tamura Takayuki , Tanaka Takaaki , Tanihata Chiharu , Tashiro Makoto , Terada Yukikatsu , Tominaga Shin’ya , Uchiyama Yasunobu , Watanabe Shin , Yamaoka Kazutaka , Yanagida Takayuki , Yonetoku Daisuke 
Published: March 2014

Abstract
The Hard X-ray Detector (HXD) on board Suzaku covers a wide energy range from 10 keV to 600 keV by the combination of silicon PIN diodes and GSO scintillators. The HXD is designed to achieve an extremely low in-orbit background based on a combination of new techniques, including the concept of a well-type active shield counter. With an effective area of $142 \,\mathrm{cm}^{2}$ at 20 keV and $273 \,\mathrm{cm}^{2}$ at 150 keV, the background level at sea level reached $\sim 1 \times 10^{-5} \,\mathrm{cts} \,\mathrm{s}^{-1} \,\mathrm{cm}^{-2} \,\mathrm{keV}^{-1}$ at 30 keV for the PIN diodes, and $\sim 2 \times 10^{-5} \,\mathrm{cts} \,\mathrm{s}^{-1} \,\mathrm{cm}^{-2} \,\mathrm{keV}^{-1}$ at 100 keV, and $\sim 7 \times 10^{-6} \,\mathrm{cts} \,\mathrm{s}^{-1} \,\mathrm{cm}^{-2} \,\mathrm{keV}^{-1}$ at 200 keV for the phoswich counter. Tight active shielding of the HXD results in a large array of guard counters surrounding the main detector parts. These anti-coincidence counters, made of $\sim 4 \,\mathrm{cm}$ thick BGO crystals, have a large effective area for sub-MeV to MeV $\gamma$-rays. They work as an excellent $\gamma$-ray burst monitor with limited angular resolution ($\sim 5^{\circ}$). The on-board signal-processing system and the data transmitted to the ground are also described.
The X-Ray Telescope onboard Suzaku
Authors: Serlemitsos Peter J. , Soong Yang , Chan Kai-Wing , Okajima Takashi , Lehan John P. , Maeda Yoshitomo , Itoh Kei , Mori Hideyuki , Iizuka Ryo , Itoh Akiharu , Inoue Hirohiko , Okada Shunsaku , Yokoyama Yushi , Itoh Yumi , Ebara Masatoshi , Nakamura Ryoko , Suzuki Kensuke , Ishida Manabu , Hayakawa Akira , Inoue Chiaki , Okuma Satoshi , Kubota Ren , Suzuki Masaki , Osawa Takeyuki , Yamashita Koujun , Kunieda Hideyo , Tawara Yuzuru , Ogasaka Yasushi , Furuzawa Akihiro , Tamura Keisuke , Shibata Ryo , Haba Yoshito , Naitou Masataka , Misaki Kazutami 
Published: March 2014

Abstract
We present the design parameters, production process, and in-flight performance of the X-ray telescope (XRT) onboard Suzaku. The imaging capability is significantly improved over the ASCA XRT, which had half-power diameters of ${3\rlap {.}{}^{\mathrm {\prime }}6}$, to ${1\rlap {.}{}^{\mathrm {\prime }}8}$–${2\rlap {.}{}^{\mathrm {\prime }}3}$ for all four XRT-I modules. The optical axes are found to be distributed within a radius of ${1\rlap {.}{}^{\mathrm {\prime }}3}$, which makes the observation efficiency of all the XRTs more than 97% at the XIS-default observing position. The vignetting over the XIS field of view predicted via ray-tracing coincides with that measured for observations of the Crab Nebula to within $\sim 10\%$. Contemporaneous fits of a power law to all of the XIS spectra of the Crab Nebula taken at the two standard observing positions (XIS/HXD-default positions) gives a flux consistent with that obtained by Toor and Seward (1974, AJ, 79, 995) to within $\sim 2\%$. The pre-collimator on the top of each XRT module successfully reduces the intensity of the stray light from the $20'$ and $50'$-off directions down to the level of pre-flight expectations.
Flight Performance of the AKARI Cryogenic System
Authors: Nakagawa Takao , Enya Keigo , Hirabayashi Masayuki , Kaneda Hidehiro , Kii Tsuneo , Kimura Yoshiyuki , Matsumoto Toshio , Murakami Hiroshi , Murakami Masahide , Narasaki Katsuhiro , Narita Masanao , Ohnishi Akira , Tsunematsu Shoji , Yoshida Seiji 
Published: March 2014

Abstract
We describe the flight performance of the cryogenic system of the infrared astronomical satellite AKARI, which was successfully launched on 2006 February 21 (UT). AKARI carries a 68.5 cm telescope together with two focal-plane instruments, Infrared Cameras and Far Infrared Surveyor, all of which are cooled down to cryogenic temperature to achieve superior sensitivity. AKARI has a unique cryogenic system, which consists of cryogen (liquid helium) and mechanical coolers (2-stage Stirling coolers). With the help of mechanical coolers, 179 L (26.0 kg) of super-fluid liquid helium can keep the instruments cryogenically cooled for more than 500 days. The on-orbit performance of the AKARI cryogenics is consistent with the design and a pre-flight test, and the boil-off gas flow rate is as small as 0.32 mg s$^{-1}$. We observed an increase in the major axis of the AKARI orbit, which can be explained by thrust due to the thermal pressure of vented helium gas.
The Far-Infrared Surveyor (FIS) for AKARI
Authors: Kawada Mitsunobu , Baba Hajime , Barthel Peter D. , Clements David , Cohen Martin , Doi Yasuo , Figueredo Elysandra , Fujiwara Mikio , Goto Tomotsugu , Hasegawa Sunao , Hibi Yasunori , Hirao Takanori , Hiromoto Norihisa , Jeong Woong-Seob , Kaneda Hidehiro , Kawai Toshihide , Kawamura Akiko , Kester Do , Kii Tsuneo , Kobayashi Hisato , Kwon Suk Minn , Lee Hyung Mok , Makiuti Sin’itirou , Matsuo Hiroshi , Matsuura Shuji , MÜller Thomas G. , Murakami Noriko , Nagata Hirohisa , Nakagawa Takao , Narita Masanao , Noda Manabu , Oh Sang Hoon , Okada Yoko , Okuda Haruyuki , Oliver Sebastian , Ootsubo Takafumi , Pak Soojong , Park Yong-Sun , Pearson Chris P. , Rowan-Robinson Michael , Saito Toshinobu , Salama Alberto , Sato Shinji , Savage Richard S. , Serjeant Stephen , Shibai Hiroshi , Shirahata Mai , Sohn Jungjoo , Suzuki Toyoaki , Takagi Toshinobu , Takahashi Hidenori , Thomson Matthew , Usui Fumihiko , Verdugo Eva , Watabe Toyoki , White Glenn J. , Wang Lingyu , Yamamura Issei , Yamauchi Chisato , Yasuda Akiko 
Published: March 2014

Abstract
The Far-Infrared Surveyor (FIS) is one of two focal-plane instruments on the AKARI satellite. FIS has four photometric bands at 65, 90, 140, and 160 $\mu \rm m$, and uses two kinds of array detectors. The FIS arrays and optics are designed to sweep the sky with high spatial resolution and redundancy. The actual scan width is more than eight arcminutes, and the pixel pitch matches the diffraction limit of the telescope. Derived point-spread functions (PSFs) from observations of asteroids are similar to those given by the optical model. Significant excesses, however, are clearly seen around tails of the PSFs, whose contributions are about 30% of the total power. All FIS functions are operating well in orbit, and the performance meets the laboratory characterizations, except for the two longer wavelength bands, which are not performing as well as characterized. Furthermore, the FIS has a spectroscopic capability using a Fourier transform spectrometer (FTS). Because the FTS takes advantage of the optics and detectors of the photometer, it can simultaneously make a spectral map. This paper summarizes the in-flight technical and operational performance of the FIS.
Properties of UIR Bands in NGC6946 Based on Mid-Infrared Imaging and Spectroscopy with Infrared Camera on Board AKARI
Authors: Sakon Itsuki , Onaka Takashi , Wada Takehiko , Ohyama Youichi , Matsuhara Hideo , Kaneda Hidehiro , Ita Yoshifusa , Ohyabu Shinki , Kataza Hirokazu , Fujishiro Naofumi , Ihara Chiaki , Ishigaki Miho , Ishihara Daisuke , Kim Woojung , Okada Yoko , Takagi Toshinobu , TanabÉ Toshihiko , Uemizu Kazunori , Ueno Munetaka , Usui Fumihiko , Watarai Hidenori , Koo Bon-Chul , Serjeant Stephen , Nakagawa Takao , Matsumoto Toshio , Murakami Hiroshi 
Published: March 2014

Abstract
We present results on mid-infrared imaging and spectroscopic observations of the nearby late-type spiral NGC6946 with the Infrared Camera on board AKARI. Based on mid-infrared imaging with the S7 (7$\mu$m) and S11(11$\mu$m) bands, we found that the S7/S11 ratios have larger values in the arm region, containing many star-forming regions, than in the interarm. Slit spectra of an interarm and a star-forming region show a series of unidentified infrared (UIR) bands at 6.2, 7.7, 8.6, and 11.2$\mu$m. The strengths of the 6.2, 7.7, and 8.6$\mu$m bands are larger relative to the 11.2$\mu$m band in the star-forming region, than in the interarm, even if the interstellar extinction of $A_V=3$mag towards the star-forming region is taken into account. The increase in the 6.2$\mu$m and 7.7$\mu$m features relative to the 11.2$\mu$m feature is consistent with the ionization model of PAHs. The ratio of the UIR features to the plateau emission under the 7.7$\mu$m and 8.6$\mu$m features and/or the ratio of the 7.6$\mu$m/7.8$\mu$m components in the 7.7$\mu$m feature increase in the star-forming region compared to the interarm. This variation can be accounted for by the hypothesis that the photo-evaporation of PAH clusters produce small free-flying PAHs in the star-forming region. The ratios of 6.2$\mu$m/11.2$\mu$m, 7.7$\mu$m/11.2$\mu$m, and 8.6$\mu$m/11.2$\mu$m may be tools to measure the star-formation activity in remote galaxies if these ratios and their variations are well examined and established for a large sample.
Multi-Wavelength Analysis of 18$\mu $m-Selected Galaxies in the AKARI/Infrared-Camera monitor field towards the North Ecliptic Pole
Authors: Takagi Toshinobu , Matsuhara Hideo , Wada Takehiko , Oyabu Shinki , Imai Koji , Pearson Chris P. , Hanami Hitoshi , Onaka Takashi , Fujishiro Naofumi , Ishihara Daisuke , Ita Yoshifusa , Kataza Hirokazu , Kim Woojung , Matsumoto Toshio , Murakami Hiroshi , Ohyama Youichi , Sakon Itsuki , TanabÉ Toshihiko , Uemizu Kazunori , Ueno Munetaka , Watarai Hidenori , Usui Fumihiko , Lee Hyung Mok , Im Myungshin , Serjeant Stephen , Savage Richard S. , Tange Tsutomu , Nakagawa Takao 
Published: March 2014

Abstract
We present an initial analysis of AKARI 18$\mu $m-selected galaxies using all 9 photometric bands at 2–24$\mu $m available in the Infrared Camera (IRC), in order to demonstrate new capabilities of AKARI cosmological surveys with this unprecedented wavelength coverage at mid-infrared (MIR) bands. We detected 72 sources at 18$\mu $m in an area of 50.2 arcmin$^2$ in the AKARI/IRC monitor field towards the North Ecliptic Pole (NEP). From this sample, 25 galaxies with probable redshifts of $z \gtrsim$ 0.5 were selected with a single colour cut (N2$-$N3$\gt$ 0.1) for a detailed spectral energy distribution (SED) analysis with ground-based $BVRi'z'JK$ data. Using an SED radiative transfer model of starbursts covering the wavelength range UV–submm, we derived photometric redshifts from the optical-MIR SEDs of 18$\mu $m-selected galaxies. From the best-fit SED models, we showed that the IRC all-band photometry is capable of tracing a steep rise in the flux at the blue side of the polycyclic aromatic hydrocarbon (PAH) 6.2$\mu $m emission feature. This indicates that the IRC all-band photometry is useful to constrain the redshift of infrared galaxies, specifically for dusty galaxies with a less prominent 4000Å break. Also, we found that the flux dip between the PAH 7.7 and 11.2$\mu $m emission feature is recognizable in the observed SEDs of galaxies at $z \sim 1$. This pilot study suggests the possibility of detecting many interesting galaxy properties in the NEP-Deep and Wide surveys, such as a systematic difference in SEDs between high–and low-$z$ Ultra-Luminous InfraRed Galaxies, and a large variation of the PAH inter-band strength ratio in galaxies at high redshifts.
Hinode SP Vector Magnetogram of AR10930 and Its Cross-Comparison with MDI
Authors: Moon Yong-Jae , Kim Yeon-Han , Park Young-Deuk , Ichimoto Kiyoshi , Sakurai Takashi , Chae Jongchul , Cho Kyung Suk , Bong Suchan , Suematsu Yoshinori , Tsuneta Saku , Katsukawa Yukio , Shimojo Masumi , Shimizu Toshifumi , Shine Richard A. , Tarbell Theodore D. , Title Alan M. , Lites Bruce , Kubo Masahito , Nagata Shin’ichi , Yokoyama Takaaki 
Published: March 2014

Abstract
We present one Hinode Spectropolarimeter (SP) magnetogram of AR 10930 that produced several major flares. The inversion from Stokes profiles to magnetic field vectors was made using the standard Milne-Eddington code. We successfully applied the Uniform Shear Method for resolving the 180$^{\circ}$ ambiguity to the magnetogram. The inversion gave very strong magnetic field strengths (near 4500 gauss) for a small portion of area in the umbra. Considering that the observed V-profile of 6301.5 Å was well-fitted as well as a direct estimation of the Zeeman splitting results in 4300–4600 gauss, we think that the field strengths should not be far from the actual value. A cross-comparison of the Hinode SP and SOHO MDI high resolution flux densities shows that the MDI flux density could be significantly underestimated by about a factor of two. In addition, it has a serious negative correlation (the so-called Zeeman saturation effect) with the Hinode SP flux density for umbral regions. Finally, we could successfully obtain a recalibrated MDI magnetogram that has been corrected for the Zeeman saturation effect using not only a pair of MDI intensity and magnetogram data simultaneously observed, but also the relationship from the cross-comparison between the Hinode SP and MDI flux densities.
Initial Helioseismic Observations by Hinode/SOT
Authors: Sekii Takashi , Kosovichev Alexander G. , Zhao Junwei , Tsuneta Saku , Shibahashi Hiromoto , Berger Thomas E. , Ichimoto Kiyoshi , Katsukawa Yukio , Lites Bruce , Nagata Shin’ichi , Shimizu Toshifumi , Shine Richard A. , Suematsu Yoshinori , Tarbell Theodore D. , Title Alan M. 
Published: March 2014

Abstract
Results from initial helioseismic observations by the Solar Optical Telescope on-board Hinode are reported. It has been demonstrated that intensity oscillation data from the Broadband Filter Imager can be used for various helioseismic analyses. The $k$–$\omega$ power spectra, as well as the corresponding time–distance cross-correlation function, which promise high-resolution time–distance analysis below the 6-Mm travelling distance, were obtained for G-band and Ca II-H data. Subsurface supergranular patterns were observed from our first time–distance analysis. The results show that the solar oscillation spectrum is extended to much higher frequencies and wavenumbers, and the time–distance diagram is extended to much shorter travel distances and times than were observed before, thus revealing great potential for high-resolution helioseismic observations from Hinode.
Hinode EUV Imaging Spectrometer Observations of Active Region Loop Morphology: Implications for Static Heating Models of Coronal Emission
Authors: Brooks David H. , Warren Harry P. , Ugarte-Urra Ignacio , Matsuzaki Keiichi , Williams David R. 
Published: March 2014

Abstract
Theoretically, magnetic fields are expected to expand as they rise above the photosphere and into the corona, so the apparent uniform cross-sections of active region loops are difficult to understand. There has been some debate as to whether coronal loops really have constant cross-sections, or are actually unresolved and composed of expanding threads within the constant cross-section envelopes. Furthermore, loop expansion is critical to the success or failure of hydrostatic models in reproducing the intensities and morphology of observed emission. We analyze Hinode EIS (EUV Imaging Spectrometer) observations of loops in active region 10953 and detect only moderate apex width expansion over a broad range of temperatures from $\log T_{\rm e}/$ K $=$ 5.6 to 6.25. The expansion is less than required by steady-state heating models of coronal emission suggesting that such models will have difficulty reproducing both low and high temperature loop emission simultaneously. At higher temperatures ($\gt \log T_{\rm e}/\gt \log T_{\rm e}/$ K $=$ 6.3) the apex widths increase substantially, but the emission at these temperatures likely comes from a combination of multiple loops. These observations demonstrate the advantage of EIS over previous instruments. For the first time, active region loops can be examined over a broad temperature range with high temperature fidelity and the same spatial resolution. The results therefore provide further clues to the coronal heating timescale and thus have implications for the direction of future modeling efforts.
Solar Transition Region Features Observed with Hinode/EIS
Authors: Young Peter R. , Zanna Del Giulio , Mason Helen E. , Doschek George A. , Culhane Len , Hara Hirohisa 
Published: March 2014

Abstract
Two types of solar active region feature prominent at transition region temperatures are identified in Hinode/EIS data of AR 10938 taken on 2007 January 20. The footpoints of 1 MK TRACE loops are shown to emit strongly in emission lines formed at $\log~T=$ 5.4–5.8, allowing the temperature increase along the footpoints to be clearly seen. A density diagnostic of Mg VII yields the density in the footpoints, with one loop showing a decrease from $3\times 10^9$ cm$^{-3}$ at the base to 1.5$\times$10$^9$ cm$^{-3}$ at a projected height of 20 Mm. The second feature is a compact active region transition region brightening which is particularly intense in O V emission ($\log~T=$ 5.4) but also has a signature at temperatures up to $\log~T=$ 6.3. The Mg VII diagnostic gives a density of $4\times 10^{10}$ cm$^{-3}$, and emission lines of Mg VI and Mg VII show line profiles broadened by 50 km s$^{-1}$ and wings extending beyond $\pm$200 km s$^{-1}$. Continuum emission in the short wavelength band is also found to be enhanced, and is suggested to be free-bound emission from recombination onto He$^+$.
Magnetic Feature and Morphological Study of X-Ray Bright Points with Hinode
Authors: Kotoku Jun’ichi , Kano Ryouhei , Tsuneta Saku , Katsukawa Yukio , Shimizu Toshifumi , Sakao Taro , Shibasaki Kiyoto , DeLuca Edward E. , Korreck Kelly E. , Golub Leon , Bobra Monica 
Published: March 2014

Abstract
We observed X-ray bright points (XBPs) in a quiet region of the Sun with the X-Ray Telescope (XRT) aboard the Hinode satellite on 2006 December 19. XRT’s high-resolution X-ray images revealed many XBPs with complicated structure and evolving dramatically with time. Almost all of the dynamic eruptions in the quiet region were composed of XBPs, and they had either loop or multiloop shapes, as is observed in larger flares. Brightening XBPs had strong magnetic fields with opposite polarities near their footpoints. While we have found a possible example of associated magnetic cancellation, other XBPs brighten and fade without any associated movement of the photospheric magnetic field.
Small-Scale X-Ray/EUV Jets Seen in Hinode XRT and TRACE
Authors: Kim Yeon-Han , Moon Young-Jae , Park Young-Deuk , Sakurai Takashi , Chae Jongchul , Cho Kyung Suk , Bong Su-Chan 
Published: March 2014

Abstract
We present the morphological and kinematic characteristics of three small-scale X-ray/EUV jets simultaneously observed by the Hinode XRT and the TRACE. For this, we examined all XRT movies with a thin Al/Poly filter from 2006 October 20 to 2007 April 8, and then found 34 small-scale eruptions. We next took a look at the corresponding TRACE 171/195 Å images associated with the eruptions. As a result, we found three simultaneous X-ray and EUV jets. For two different bands, they have similar characteristics in terms of the projected speed (90–310 km s$^{-1}$), lifetime (100–2000 s), and size (1.1–5$\times$10$^5$km). These characteristics are similar to the previous results by the Yohkoh SXT, but are quite different from EUV jets associated with H$\alpha$ surges. From the EUV Imaging Spectrometer, four spectral lines for the last event, we found blueshift (up to $-$64 km s$^{-1}$) and redshift (up to 20 km s$^{-1}$) motions as well as nonthermal velocities ranging from 57 to 106 km s$^{-1}$ at the jet footpoint. We note a tendency: the hotter the maximum ionization temperature is, the smaller the area of blueshift region is. These characteristics are consistent with a typical jet model that includes the magnetic reconnection between open coronal fields and emerging magnetic fields.
Hinode Observations of a Vector Magnetic Field Change Associated with a Flare on 2006 December 13
Authors: Kubo Masahito , Yokoyama Takaaki , Katsukawa Yukio , Lites Bruce , Tsuneta Saku , Suematsu Yoshinori , Ichimoto Kiyoshi , Shimizu Toshifumi , Nagata Shin’ichi , Tarbell Theodore D. , Shine Richard A. , Title Alan M. , Elmore David 
Published: March 2014

Abstract
Continuous observations of the flare productive active region 10930 were successfully carried out with the Solar Optical Telescope aboard the Hinode spacecraft during 2006 December 6 to 19. We focused on the evolution of photospheric magnetic fields in this active region, and the magnetic field properties at the site of the X3.4 class flare, using a time series of vector field maps with high spatial resolution. The X3.4 class flare occurred on 2006 December 13 at the apparent collision site between the large, opposite polarity umbrae. Elongated magnetic structures with alternatingly positive and negative polarities resulting from flux emergence appeared one day before the flare in the collision site penumbra. Subsequently, the polarity inversion line at the collision site became very complicated. The number of bright loops in Ca II H increased during the formation of these elongated magnetic structures. Flare ribbons and bright loops evolved along the polarity inversion line and one footpoint of the bright loop was located in a region having a large departure of the field azimuth angle with respect to its surroundings. SOT observations with high spatial resolution and high polarization precision revealed temporal change in the fine structure of magnetic fields at the flare site: some parts of the complicated polarity inversion line then disappeared, and in those regions the azimuth angle of the photospheric magnetic field changed by about 90°, becoming more spatially uniform within the collision site.