Commissioning status of Subaru laser guide star adaptive optics system

Hayano, Yutaka; Takami, Hideki; Oya, Shin; Hattori, Masayuki; Saito, Yoshihiko; Watanabe, Makoto; Guyon, Olivier; Minowa, Yosuke; Egner, Sebastian; Ito, Meguru; Garrel, Vincent; Colley, Stephen; Golota, Taras; Iye, Masanori

doi:10.1117/12.857567

Cited by 96 publications

(31 citation statements)

References 18 publications

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“…We obtained high-resolution J-band image of TXS 2116−077 with the InfraRed Camera and Spectrograph (IRCS; Kobayashi et al 2000), in combination with its adaptive optics (AO) system AO188 (Hayano et al 2010), mounted at the Subaru Telescope on 2018 June 16. We used a resolution of 0.052 per pixel for a corresponding 54 field of view.…”

Section: Host Galaxy Imaging With Subarumentioning

confidence: 99%

TXS 2116−077: A Gamma-Ray Emitting Relativistic Jet Hosted in a Galaxy Merger

Paliya

Pérez

García-Benito

et al. 2020

ApJ

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What triggers collimated relativistic outflows or jets, from the centers of galaxies remains a fundamental question in astrophysics. The merging of two galaxies has been proposed to realize the conditions to successfully launch and drive such jets into the intergalactic medium. However, evidences for the operation of this mechanism are scarce. Here we report the first unambiguous detection of an ongoing merger of a narrow-line Seyfert 1 galaxy, TXS 2116−077, hosting a closely aligned, γ-ray emitting relativistic jet with a Seyfert 2 galaxy at a separation of ∼12 kpc, using the observations taken with 8.2 m Subaru telescope. Our subsequent followup observations with 10.4 m Gran Telescopio Canarias, 4.2 m William Herschel Telescope, and Chandra X-ray observatory have provided what is likely to be the first glimpse of the merging environment hosting a closely aligned relativistic jet. Our finding that the jet is considerably younger than the merger demonstrates that jet activity can be triggered by galaxy mergers and that γ-ray detected narrow-line Seyfert 1 galaxies represent the beginning phase of that activity. These results also highlight the crucial role of mergers in shaping the fate of galaxies in their cosmological evolution and are consistent with recent studies focused on the host galaxy imaging of this enigmatic class of active galactic nuclei.

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Section: Host Galaxy Imaging With Subarumentioning

confidence: 99%

TXS 2116−077: A Gamma-Ray Emitting Relativistic Jet Hosted in a Galaxy Merger

Paliya

Pérez

García-Benito

et al. 2020

ApJ

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“…Its detector is a 1024 × 1024 InSb array with a pixel resolution of 0.053 × 0.053 arcsec 2 (160 × 160 km 2 at Jupiter). In this paper, we analyzed the three data sets listed in Table 1 when the 188-element Adaptive Optics module (AO188) [Hayano et al, 2008[Hayano et al, , 2010Minowa et al, 2010] was activated. Figure 1 shows an example of an observed spectrum (AO2 in Table 1).…”

Section: Observation and Data Reductionmentioning

confidence: 99%

Vertical emissivity profiles of Jupiter's northern H₃⁺ and H₂ infrared auroras observed by Subaru/IRCS

et al. 2014

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We resolved the vertical emissivity profiles of H 3 + overtone, H 3 + hot overtone, and H 2 emission lines of the Jovian northern auroras in K band obtained in December 2011 observed by the IR Camera and Spectrograph of the Subaru 8.2 m telescope with the adaptive optics system (AO188). The spatial resolution achieved was~0.2 arcsec, corresponding to~600 km at Jupiter. We derived the vertical emissivity profiles at three polar regions close to the Jovian limb. The H 3 + overtone and H 3 + hot overtone lines had similar peak altitudes of 700-900 km and 680-950 km above the 1 bar level, which were 100-300 km and 150-420 km lower, respectively, than the model values. On the contrary, the H 2 peak emission altitude was high, 590-720 km above the 1 bar level. It was consistent with the value expected for precipitation of~1 keV electron, which favors a higher-altitude emissivity profile. We concluded that the lower peak altitudes of H 3 + overtone and hot overtone lines were caused by the nonlocal thermodynamic equilibrium effect stronger than the model assumption. We could reproduce the observational emissivity profiles from the model by including this effect. It has been proposed that neutral H 2 and ionized H 3 + emissions can have different source altitudes because of their different morphologies and velocities; however, our observed results with a general circulation model show that the peak emission altitudes of H 3 + and H 2 can be similar even with different velocities.

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“…The adaptive optics system AO188 (Hayano et al 2010) was used to reduce the image degradation caused by atmospheric turbulence and improve the Strehl ratio. AO188ʼs atmospheric dispersion corrector (ADC; Egner et al 2010) removed the chromaticity of atmospheric refraction.…”

Section: Strategic Exploration Of Exoplanets and Disks With Subaru (Smentioning

confidence: 99%

Seeds Direct Imaging of the Rv-Detected Companion to V450 Andromedae, and Characterization of the System

Hełminiak

Kuzuhara

Mede

et al. 2016

ApJ

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We report the direct imaging detection of a low-mass companion to a young, moderately active star V450And, that was previously identified with the radial velocity (RV) method. The companion was found in high-contrast images obtained with the Subaru Telescope equipped with the HiCIAO camera and AO188 adaptive optics system. From the public ELODIE and SOPHIE archives we extracted available high-resolution spectra and RV measurements, along with RVs from the Lick planet search program. We combined our multi-epoch astrometry with these archival, partially unpublished RVs, and found that the companion is a low-mass star, not a brown dwarf, as previously suggested. We found the best-fitting dynamical masses to be = M . We also performed spectral analysis of the SOPHIE spectra with the iSpec code. Hipparcos time-series photometry shows a periodicity of P=5.743 day, which is also seen in the SOPHIE spectra as an RV modulation of the star A. We interpret it as being caused by spots on the stellar surface, and the star to be rotating with the given period. From the rotation and level of activity, we found that the system is -+ 380 100 220 Myr old, consistent with an isochrone analysis ( -+ 220 90 2120 Myr). This work may serve as a test case for future studies of lowmass stars, brown dwarfs, and exoplanets by combination of RV and direct imaging data.

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Commissioning status of Subaru laser guide star adaptive optics system

Cited by 96 publications

References 18 publications

TXS 2116−077: A Gamma-Ray Emitting Relativistic Jet Hosted in a Galaxy Merger

TXS 2116−077: A Gamma-Ray Emitting Relativistic Jet Hosted in a Galaxy Merger

Vertical emissivity profiles of Jupiter's northern H₃⁺ and H₂ infrared auroras observed by Subaru/IRCS

Seeds Direct Imaging of the Rv-Detected Companion to V450 Andromedae, and Characterization of the System

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Commissioning status of Subaru laser guide star adaptive optics system

Cited by 96 publications

References 18 publications

TXS 2116−077: A Gamma-Ray Emitting Relativistic Jet Hosted in a Galaxy Merger

TXS 2116−077: A Gamma-Ray Emitting Relativistic Jet Hosted in a Galaxy Merger

Vertical emissivity profiles of Jupiter's northern H3+ and H2 infrared auroras observed by Subaru/IRCS

Seeds Direct Imaging of the Rv-Detected Companion to V450 Andromedae, and Characterization of the System

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Product

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About

Vertical emissivity profiles of Jupiter's northern H₃⁺ and H₂ infrared auroras observed by Subaru/IRCS