Current Performance and On-Going Improvements of the 8.2 m Subaru Telescope

Iye, Masanori; Karoji, Hiroshi; Ando, Hiroyasu; Kaifu, Norio; Kodaira, Keiichi; Aoki, Kentaro; Aoki, Wako; Chikada, Yoshihiro; Doi, Yoshihiro; Ebizuka, Noboru; Elms, Brian; Fujihara, G.; Furusawa, Hisanori; Fuse, Tetsuharu; Gäessler, Wolfgang; Harasawa, S.; Hayano, Yutaka; Hayashi, Masahiko; Hayashi, Saeko S.; Ichikawa, Shinichi; Imanishi, Masatoshi; Ishida, C. M.; Kamata, Yukiko; Kanzawa, Tomio; Kashikawa, Nobunari; Kawabata, Koji S.; Kobayashi, Naoto; Komiyama, Yutaka; Kosugi, George; Kurakami, Tomio; Letawsky, Michael; Mikami, Yoshitaka; Miyashita, Akihiko; Miyazaki, Satoshi; Mizumoto, Y.; Morino, Jun-Ichi; Motohara, Kentaro; Murakawa, K.; Nakagiri, M.; Nakamura, Kyoko; Nakaya, Hidehiko; Nariai, Kyoji; Nishimura, Tetsuo; Noguchi, Kunio; Noguchi, T.; Noumaru, Junichi; Ogasawara, Ryusuke; Ohshima, Norio; Ohyama, Youichi; Okita, Kiichi; Omata, K.; Otsubo, Masahisa; Oya, Shin; Potter, Robert D.; Saito, Yoshihiko; Sasaki, Toshiyuki; Sato, Shuji; Scarla, D.; Schubert, Kiaina; Sekiguchi, Kazuhiko; Sekiguchi, M.; Shelton, Ian; Simpson, Chris; Shimada, Hiroshi; Tajitsu, Akito; Takami, Hideki; Takata, Tadafumi; Takato, Naruhisa; Tamae, Richard; Tamura, Motohide; Tanaka, Wataru; Terada, Hiroshi; Torii, Yasuo; Uraguchi, Fumihiko; Usuda, Tomonori; Weber, Mark; Winegar, Tom; Yagi, Masafumi; Yamada, Tōru; Yamashita, Takuya; Yamashita, Yasumasa; Yasuda, Naoki; Yoshida, Michitoshi; Yutani, Masami

doi:10.1093/pasj/56.2.381

Cited by 145 publications

(66 citation statements)

References 70 publications

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“…We briefly describe our observations and data reduction, although the details will be reported in a separate paper (Yamada et al, in preparation). The summary of the observations and data is listed in (Iye et al 2004). Suprime-Cam has a pixel scale of 0.2 arcsec and a field of view of 34 × 27 arcmin 2 .…”

Section: O B S E Rvat I O N S a N D Data R E D U C T I O Nmentioning

confidence: 99%

The Subaru Lyα blob survey: a sample of 100-kpc Lyα blobs at z = 3

Matsuda

Yamada

Hayashino

et al. 2011

Monthly Notices of the Royal Astronomical Society: Letters

133

166

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We present results of a survey for giant Lyα blobs (LABs) at z= 3 with Subaru/Suprime‐Cam. We obtained Lyα imaging at z= 3.09 ± 0.03 around the SSA22 protocluster and in several blank fields. The total survey area is 2.1 deg2, corresponding to a comoving volume of 1.6 × 106 Mpc3. Using a uniform detection threshold of 1.4 × 10−18 erg s−1 cm−2 arcsec−2 for the Lyα images, we construct a sample of 14 LAB candidates with major‐axis diameters larger than 100 kpc, including five previously known blobs and two known quasars. This survey triples the number of known LABs over 100 kpc. The giant LAB sample shows a possible ‘morphology–density relation’: filamentary LABs reside in average density environments as derived from compact Lyα emitters, while circular LABs reside in both average density and overdense environments. Although it is hard to examine the formation mechanisms of LABs only from the Lyα morphologies, more filamentary LABs may relate to cold gas accretion from the surrounding intergalactic medium (IGM) and more circular LABs may relate to large‐scale gas outflows, which are driven by intense starbursts and/or by active galactic nucleus activities. Our survey highlights the potential usefulness of giant LABs to investigate the interactions between galaxies and the surrounding IGM from the field to overdense environments at high redshift.

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Section: O B S E Rvat I O N S a N D Data R E D U C T I O Nmentioning

confidence: 99%

The Subaru Lyα blob survey: a sample of 100-kpc Lyα blobs at z = 3

Matsuda

Yamada

Hayashino

et al. 2011

Monthly Notices of the Royal Astronomical Society: Letters

133

166

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“…We obtained narrow-and broad-band imaging centred at (α, δ) = 13:11:29.5, −01:20:17 (J2000.0) on 2009 May 23-24 (UT) using Suprime-Cam (Miyazaki et al 2002) on the 8.2-m Subaru Telescope (Iye et al 2004) as an open use normal programme (S09A−104). We also used archival V-band data of the same field taken on 2001 April 24 (UT).…”

Section: O B S E Rvat I O N S a N D Data R E D U C T I O Nmentioning

confidence: 99%

A search for galaxies in and around an HI overdense region at z = 5

Matsuda¹,

Richard²,

Smail³

et al. 2010

Monthly Notices of the Royal Astronomical Society: Letters

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We present the discovery of a large‐scale structure of emission‐line galaxies at redshift z= 4.86 behind a massive cluster of galaxies, A1689. Previous spectroscopic observations of a galaxy, A1689−7.1 at z= 4.87, near this structure, revealed a possible overdense region of intergalactic medium (IGM) around the galaxy, which extends at least ∼80 comoving Mpc along the line of sight. In order to investigate whether this z∼ 5 IGM overdense region contains a galaxy overdensity, we undertook narrow‐ and broad‐band imaging observations around A1689−7.1 with Subaru/Suprime‐Cam. We detected 51 candidates as Lyα emitters at redshift z= 4.86 ± 0.03 in the 32 × 24 arcmin2 field of view. After correction for lensing by the foreground cluster, we found a large‐scale (∼20 × 60 comoving Mpc) overdense region of galaxies around A1689−7.1 in the source plane at z= 4.86. The densest peak in this region has an overdensity of δ∼ 4, suggesting that this structure is probably a good candidate for a protocluster which may evolve into a massive cluster of galaxies in the present‐day Universe. A1689−7.1 is located at the edge of this region, where the local galaxy density is ∼1.6 times the mean density and is close to the density contrast in the IGM along the line of sight to A1689−7.1 estimated from the optical depth. The overdensities of galaxies we have found may suggest that at least some parts of the IGM overdense region have already started to form galaxies and moreover they relate to the formation of a protocluster. Although we lack information on the three‐dimensional distributions of both IGM and galaxy overdense regions, the similarity of the scales of both regions may suggest that the two are parts of a single large‐scale structure, which would be an large edge‐on sheet along the line of sight with a size of ∼20 × 60 × 80 comoving Mpc.

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“…IRHS (mid-InfRared High dispersion Spectrograph, tentative name), candidate of second generations instrument of the 8.2 m Subaru Telescope (National Astronomical Observatory of Japan: NAOJ) [4,5], is aiming R ~ 200,000 at 10µm in order to observe vibrational transitions of molecule in circum-stellar and dark clouds for instance. IRHS requires a disperser with minimum 2 m in an optical path difference.…”

Section: Novel Immersion Gratingmentioning

confidence: 99%

Novel immersion grating, VPH grating and quasi-Bragg grating

et al. 2006

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We have successfully fabricated germanium immersion gratings with resolving power of 45,000 at 10 µm by using a nano precision 3D grinding machine and ELID (ELectrolytic In-process Dressing) method. However the method spends large amount of machine times. We propose grooves shape with a new principle for a solid grating, which achieves high performance and lower cost.We have developed volume phase holographic (VPH) grisms with zinc selenide (ZnSe) prisms for spectrograph of the Subaru Telescope and the other telescopes. While a VPH grism with high index prisms achieves higher dispersion, diffraction efficiency of VPH grating decreases toward higher orders. A "quasi-Bragg grating" which inherits advantage of a VPH grating achieves high diffraction efficiency toward higher orders.Wavelength tuners with a pair of counter-rotation prisms for a VPH and quasi-Bragg grating obtain high diffraction efficiency over wide wavelength range. The novel immersion grating, VPH grism with high index prisms, quasi-Bragg grating and wavelength tuners dramatically reduce volumes of astronomical spectrographs.

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Current Performance and On-Going Improvements of the 8.2 m Subaru Telescope

Cited by 145 publications

References 70 publications

The Subaru Lyα blob survey: a sample of 100-kpc Lyα blobs at z = 3

The Subaru Lyα blob survey: a sample of 100-kpc Lyα blobs at z = 3

A search for galaxies in and around an HI overdense region at z = 5

Novel immersion grating, VPH grating and quasi-Bragg grating

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