Development of the Wide Field Grism Spectrograph 2

Uehara, Mari; Nagashima, Chie; Sugitani, Koji; Watanabe, Makoto; Sato, Shuji; Nagata, T.; Tamura, Motohide; Ebizuka, Noboru; Pickles, Andrew; Hodapp, Klaus W.; Itoh, Yoichi; Nakano, Makoto; Ogura, K.

doi:10.1117/12.551055

Cited by 23 publications

(5 citation statements)

References 4 publications

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“…Slitless grism spectroscopy and g (482.5 nm), i (767.2 nm), and wide Hα (651 nm) imaging of BRC37 were conducted on UT 2006 November 19 and V , and I C imaging was done on UT 2007 August 7 with the Wide Field Grism Spectrograph 2 (WFGS2; Uehara et al 2004) mounted on the University of Hawaii 2.2 m telescope (UH88). The detector used was a Tektronix 2048 × 2048 CCD.…”

Section: Optical Observationsmentioning

confidence: 99%

Sequential Star Formation in a Cometary Globule (Brc37) of Ic1396

Ikeda

Sugitani

Watanabe

et al. 2008

The Astronomical Journal

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We have carried out near-IR/optical observations to examine star formation toward a bright-rimmed cometary globule (BRC37) facing the exciting star(s) of an H ii region (IC1396) containing an IRAS source, which is considered to be an intermediate-mass protostar. With slitless spectroscopy we detected ten Hα emission stars around the globule, six of which are near the tip of the globule and are aligned along the direction to the exciting stars. There is evidence that this alignment was originally toward an O9.5 star, but has evolved to align toward a younger O6 star when that formed. Near-IR and optical photometry suggests that four of these six stars are low-mass young stellar objects (YSOs) with masses of ∼0.4 M . Their estimated ages of ∼1 Myr indicate that they were formed at the tip in advance of the formation of the IRAS source. Therefore, it is likely that sequential star formation has been taking place along the direction from the exciting stars toward the IRAS source, due to the UV impact of the exciting star(s). Interestingly, one faint, Hα emission star, which is the closest to the exciting star(s), seems to be a young brown dwarf that was formed by the UV impact in advance of the formation of other YSOs at the tip.

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Section: Optical Observationsmentioning

confidence: 99%

Sequential Star Formation in a Cometary Globule (Brc37) of Ic1396

Ikeda

Sugitani

Watanabe

et al. 2008

The Astronomical Journal

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“…We have also fabricated a VPH grism with ZnSe prisms for WFGS 2 (Wide Field Grism Spectrograph) of the 2.2m Telescope of the University of Hawaii [30]. And VPH grisms with ZnSe prisms for MOIRCS (Multi-Object InfraRed Camera and Spectrograph) [31] of the Subaru Telescope are under developing.…”

Section: Vph Grism With High Index Prismsmentioning

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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“…Spectral Imager (MSI; Watanabe et al 2012) mounted on the 1.6 m Pirka Telescope at NO, the Wide Field Grism Spectrograph 2 (WFGS2; Uehara et al 2004;Kawakami et al 2021) mounted on the 2.0 m Nayuta Telescope at NHAO, and the Hiroshima Optical and Near-InfraRed Camera (HONIR; Akitaya et al 2014) mounted on the 1.5 m Kanata telescope at HHO. Wollaston prisms and rotatable half-wave plates are installed in all three instruments; thus, data obtained at the three sites were analyzed in the same standard reduction procedure (e.g., Kawabata et al 1999;Ishiguro et al 2017).…”

Section: Polarimetric Observationsmentioning

confidence: 99%

Photometry and Polarimetry of 2010 XC₁₅: Observational Confirmation of E-type Near-Earth Asteroid Pair

Beniyama,

Sako,

Ohtsuka

et al. 2023

ApJ

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Asteroid systems such as binaries and pairs are indicative of the physical properties and dynamical histories of small solar system bodies. Although numerous observational and theoretical studies have been carried out, the formation mechanism of asteroid pairs is still unclear, especially for near-Earth asteroid (NEA) pairs. We conducted a series of optical photometric and polarimetric observations of a small NEA 2010 XC15 in 2022 December to investigate its surface properties. The rotation period of 2010 XC15 is possibly a few to several dozen hours and the color indices of 2010 XC15 are derived as g − r = 0.435 ± 0.008, r − i = 0.158 ± 0.017, and r − z = 0.186 ± 0.009 in the Pan-STARRS system. The linear polarization degrees of 2010 XC15 are a few percent at the phase angle range of 58°–114°. We found that 2010 XC15 is a rare E-type NEA on the basis of its photometric and polarimetric properties. Taking the similarity of not only physical properties but also dynamical integrals and the rarity of E-type NEAs into account, we suppose that 2010 XC15 and 1998 WT24 are of common origin (i.e., an asteroid pair). These two NEAs are the sixth NEA pair and first E-type NEA pair ever confirmed, possibly formed by rotational fission. We conjecture that the parent body of 2010 XC15 and 1998 WT24 was transported from the main belt through the ν 6 resonance or Hungaria region.

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Development of the Wide Field Grism Spectrograph 2

Cited by 23 publications

References 4 publications

Sequential Star Formation in a Cometary Globule (Brc37) of Ic1396

Sequential Star Formation in a Cometary Globule (Brc37) of Ic1396

Novel immersion grating, VPH grating and quasi-Bragg grating

Photometry and Polarimetry of 2010 XC₁₅: Observational Confirmation of E-type Near-Earth Asteroid Pair

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Development of the Wide Field Grism Spectrograph 2

Cited by 23 publications

References 4 publications

Sequential Star Formation in a Cometary Globule (Brc37) of Ic1396

Sequential Star Formation in a Cometary Globule (Brc37) of Ic1396

Novel immersion grating, VPH grating and quasi-Bragg grating

Photometry and Polarimetry of 2010 XC15: Observational Confirmation of E-type Near-Earth Asteroid Pair

Contact Info

Product

Resources

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Photometry and Polarimetry of 2010 XC₁₅: Observational Confirmation of E-type Near-Earth Asteroid Pair