OSIRIS: a diffraction limited integral field spectrograph for Keck

Larkin, James E.; Barczys, M.; Krabbe, A.; Adkins, Sean M.; Aliado, Ted; Amico, Paola; Brims, George; Campbell, Randy; Canfield, John; Gasaway, Thomas M.; Honey, Allan; Iserlohe, C.; Johnson, Chris A.; Kress, Evan; Lafrenière, David; Lyke, James E.; Magnone, Kenneth; Magnone, Nick; McElwain, Michael; Moon, Juleen; Quirrenbach, A.; Skulason, Gunnar E.; Song, Inseok; Spencer, Michael; Weiss, Jason; Wright, Shelley A.

doi:10.1117/12.672061

Cited by 135 publications

(54 citation statements)

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“…Kuzuhara et al presented low-resolution NIR spectroscopy of this object; here we present the first moderate-resolution NIR spectrum. Tau b,ROXs 42B b, We observed FW Tau b with the OH-Suppressing Infrared Imaging Spectrograph (OSIRIS; Larkin et al 2006) on 2011 October 4 UT with the Keck II 10 m telescope using natural guide star adaptive optics (NGSAO). The 50 mas plate scale was used for both the Hbb (1.473-1.803 μm) and Kbb (1.965-2.381 μm) filters, resulting in a 0.…”

Section: Introductionmentioning

confidence: 99%

Spectroscopic Confirmation of Young Planetary-Mass Companions on Wide Orbits

Bowler

Liu

Kraus

et al. 2014

ApJ

102

110

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We present moderate-resolution (R ∼ 4000-5000) near-infrared integral field spectroscopy of the young (1-5 Myr) 6-14 M Jup companions ROXs 42B b and FW Tau b obtained with Keck/OSIRIS and Gemini-North/NIFS. The spectrum of ROXs 42B b exhibits clear signs of low surface gravity common to young L dwarfs, confirming its extreme youth, cool temperature, and low mass. Overall, it closely resembles the free-floating 4-7 M Jup L-type Taurus member 2MASS J04373705+2331080. The companion to FW Tau AB is more enigmatic. Our optical and near-infrared spectra show strong evidence of outflow activity and disk accretion in the form of line emission from, Paβ, and H 2 . The molecular hydrogen emission is spatially resolved as a single lobe that stretches ≈0. 1 (15 AU). Although the extended emission is not kinematically resolved in our data, its morphology resembles shock-excited H 2 jets primarily seen in young Class 0 and Class I sources. The near-infrared continuum of FW Tau b is mostly flat and lacks the deep absorption features expected for a cool, late-type object. This may be a result of accretion-induced veiling, especially in light of its strong and sustained Hα emission (EW(Hα) 290 Å). Alternatively, FW Tau b may be a slightly warmer (M5-M8) accreting low-mass star or brown dwarf (0.03-0.15 M ) with an edge-on disk. Regardless, its young evolutionary stage is in stark contrast to its Class III host FW Tau AB, indicating a more rapid disk clearing timescale for the host binary system than for its wide companion. Finally, we present near-infrared spectra of the young (∼2-10 Myr) low-mass (12-15 M Jup ) companions GSC 6214-210 B and SR 12 C and find they best resemble low-gravity M9.5 and M9 substellar templates.

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Section: Introductionmentioning

confidence: 99%

Spectroscopic Confirmation of Young Planetary-Mass Companions on Wide Orbits

Bowler

Liu

Kraus

et al. 2014

ApJ

102

110

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“…Yuan et al (2011) used the integral field spectrograph (IFS) OSIRIS (Larkin et al 2006) on the Keck Telescope to trace the Hα-[N ii] emission in one of the multiple images (M1 in Figure 1) of Sp1149 and found a maximum rotation velocity V max = 210 km/s (assuming an inclination of 45…”

Section: Introductionmentioning

confidence: 99%

Kinematics of the SN Refsdal host revealed by MUSE: a regularly rotating spiral galaxy at z ≃ 1.5

Teodoro

Grillo

Fraternali

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We use Multi Unit Spectroscopic Explorer (MUSE) observations of the galaxy cluster MACS J1149.5+2223 to explore the kinematics of the grand-design spiral galaxy (Sp1149) hosting the SN "Refsdal". Sp1149 lies at z 1.49, has a stellar mass M * 5×10 9 M , a star-formation rate SFR 1 − 6 M yr −1 and represents a likely progenitor of a Milky-Way-like galaxy. All the four multiple images of Sp1149 in our data show strong [O ii]-line emissions pointing to a clear rotation pattern. We take advantage of the gravitational lensing magnification effect ( 4×) on the [O ii] emission of the least distorted image to fit 3D kinematic models to the MUSE data-cube and derive the rotation curve and the velocity dispersion profile of Sp1149. We find that the rotation curve steeply rises, peaks at R 1 kpc and then (initially) declines and flattens to an average V flat = 128 +29 −19 km/s. The shape of the rotation curve is well determined but the actual value of V flat is quite uncertain because of the nearly face-on configuration of the galaxy. The intrinsic velocity dispersion due to gas turbulence is almost constant across the entire disc with an average of 27 ± 5 km/s. This value is consistent with z = 0 measurements in the ionized gas component and a factor 2-4 lower than other estimates in different galaxies at similar redshifts. The average stellar-to-total mass fraction is of the order of one fifth. Our kinematic analysis returns the picture of a regular star-forming, mildly turbulent, rotationdominated (V/σ 5) spiral galaxy in a 4 Gyr old Universe.

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“…The OSIRIS integral field spectrograph (IFS) [13] was commissioned at WMKO in 2005. OSIRIS is a near-IR IFS covering the wavelength range of 1 to 2.4 µm, with spatial sampling scales of 20, 35, 50, and 100 milli-arcseconds (mas).…”

Section: Upgrades To Osirismentioning

confidence: 99%

New developments in instrumentation at the W. M. Keck Observatory

et al. 2014

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The W. M. Keck Observatory continues to develop new capabilities in support of our science driven strategic plan which emphasizes leadership in key areas of observational astronomy. This leadership is a key component of the scientific productivity of our observing community and depends on our ability to develop new instrumentation, upgrades to existing instrumentation, and upgrades to supporting infrastructure at the observatory. In this paper we describe the as measured performance of projects completed in 2014 and the expected performance of projects currently in the development or construction phases. Projects reaching completion in 2014 include a near-IR tip/tilt sensor for the Keck I adaptive optics system, a new center launch system for the Keck II laser guide star facility, and NIRES, a near-IR Echelle spectrograph for the Keck II telescope. Projects in development include a new seeing limited integral field spectrograph for the visible wavelength range called the Keck Cosmic Web Imager, a deployable tertiary mirror for the Keck I telescope, upgrades to the spectrograph detector and the imager of the OSIRIS instrument, and an upgrade to the telescope control systems on both Keck telescopes.

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OSIRIS: a diffraction limited integral field spectrograph for Keck

Cited by 135 publications

References 0 publications

Spectroscopic Confirmation of Young Planetary-Mass Companions on Wide Orbits

Spectroscopic Confirmation of Young Planetary-Mass Companions on Wide Orbits

Kinematics of the SN Refsdal host revealed by MUSE: a regularly rotating spiral galaxy at z ≃ 1.5

New developments in instrumentation at the W. M. Keck Observatory

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