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; Magnone, Kenneth; Magnone, Nick; McElwain, Michael; Moon, Juleen; Quirrenbach, A.; Skulason, Gunnar E.; Song, Inseok; Spencer, Michael; Weiss, Jason; Wright, Shelley A.

doi:10.1016/j.newar.2006.02.005

Cited by 127 publications

(120 citation statements)

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“…OSIRIS delivers spectra simultaneously over a contiguous two-dimensional (2D) field of view (FOV) in the wavelength range from 1.1 to 2.45 μm at a resolving power of 1500-4000 (Larkin et al 2006, van Dam et al 2004, Wizinowich et al 2006. In all cases we used the galaxy nucleus as the tip-tilt star, and the 0 1 pixel scale.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

The Nature of Active Galactic Nuclei With Velocity Offset Emission Lines*

Müller–Sánchez

Comerford

Stern

et al. 2016

ApJ

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We obtained Keck/OSIRIS near-IR adaptive optics-assisted integral-field spectroscopy to probe the morphology and kinematics of the ionized gas in four velocity-offset active galactic nuclei (AGNs) from the Sloan Digital Sky Survey. These objects possess optical emission lines that are offset in velocity from systemic as measured from stellar absorption features. At a resolution of ∼0 18, OSIRIS allows us to distinguish which velocity offset emission lines are produced by the motion of an AGN in a dual supermassive black hole system, and which are produced by outflows or other kinematic structures. In three galaxies, J1018+2941, J1055+1520, and J1346+5228, the spectral offset of the emission lines is caused by AGN-driven outflows. In the remaining galaxy, J1117+6140, a counterrotating nuclear disk is observed that contains the peak of Paα emission 0 2 from the center of the galaxy. The most plausible explanation for the origin of this spatially and kinematically offset peak is that it is a region of enhanced Paα emission located at the intersection zone between the nuclear disk and the bar of the galaxy. In all four objects, the peak of ionized gas emission is not spatially coincident with the center of the galaxy as traced by the peak of the near-IR continuum emission. The peaks of ionized gas emission are spatially offset from the galaxy centers by 0 1-0 4 (0.1-0.7 kpc). We find that the velocity offset originates at the location of this peak of emission, and the value of the offset can be directly measured in the velocity maps. The emission-line ratios of these four velocity-offset AGNs can be reproduced only with a mixture of shocks and AGN photoionization. Shocks provide a natural explanation for the origin of the spatially and spectrally offset peaks of ionized gas emission in these galaxies.

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Section: Observations and Data Reductionmentioning

confidence: 99%

The Nature of Active Galactic Nuclei With Velocity Offset Emission Lines*

Müller–Sánchez

Comerford

Stern

et al. 2016

ApJ

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“…19 The uncertainties given here on the (M bh -σ)-derived black hole masses are based on an assumed 10% uncertainty on the velocity dispersion, and 0.3 dex of intrinsic scatter in the M log bh ( ) direction about the M bh -σ relation. (Larkin et al 2006) with the Keck I Laser Guide Star Adaptive Optics (LGSAO) system (Wizinowich et al 2006;van Dam et al 2006). OSIRIS is a lenslet array, integral field unit spectrograph with a 2048 × 2048 Hawaii-2 detector.…”

Section: Expected Black Hole Massmentioning

confidence: 99%

A Normal Supermassive Black Hole in Ngc 1277

Graham

Durré

Savorgnan

et al. 2016

ApJ

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The identification of galaxies with "overly massive" black holes requires two measurements: a black hole mass (M bh ) and a host spheroid mass (M sph,* ). Here we provide our measurements for NGC1277. Our structural decomposition reveals that NGC1277 is dominated by a "classical" spheroid with a Sérsic index n=5.3, a half-light radius R 2.1 kpc e,major = , and a stellar mass of M 2.7 10 11  (using M L 11.65). This mass is an order of magnitude greater than originally reported. Using the latest M bh -n, M bh -M sph,* , and M bh -σ relations, the expected black hole mass is, respectively, ( ) for which the "sphere-of-influence" is 0 31. Our new kinematical maps obtained from laser guide star assisted, adaptive optics on the Keck I Telescope dramatically reaffirm the presence of the inner, nearly edge-on, disk seen in the galaxy image. We also report that this produces a large velocity shear (∼400 km s s + across the inner 3. 8 0. 6 ( ) ( )  ´  region of the galaxy. Our new multi-Gaussian expansion (MGE) models and Jeans Anisotropic MGE analysis struggled to match this extended component. Our optimal black hole mass, albeit a probable upper limit because of the disk is). This is an order of magnitude smaller than originally reported and 4 times smaller than recently reported. It gives an M M bh sph,* ratio of 0.45% in agreement with the median (≈0.5%) and range (0.1%-5.0%) observed in non-dwarf, early-type galaxies. This result highlights the need for caution with inner disks.

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“…H ii 1348 was also targeted as part of a demonstration project for the then newly commissioned OSIRIS integral field spectrograph (Larkin et al 2006). We obtained 1.18-1.35 μm (Jbb) and 1.47-1.80 μm (Hbb) diffraction-limited integral field spectra of the pair with the Keck AO system (Wizinowich et al 2000) on 2005 November 21.…”

Section: Astrometry and Photometrymentioning

confidence: 99%

A Substellar Common Proper-Motion Companion to the Pleiad H Ii 1348

Geißler

Metchev

Pham

et al. 2012

ApJ

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We announce the identification of a proper-motion companion to the star H ii 1348, a K5 V member of the Pleiades open cluster. The existence of a faint point source 1. 1 away from H ii 1348 was previously known from adaptive optics imaging by Bouvier et al. However, because of a high likelihood of background star contamination and in the absence of follow-up astrometry, Bouvier et al. tentatively concluded that the candidate companion was not physically associated with H ii 1348. We establish the proper-motion association of the pair from adaptive optics imaging with the Palomar 5 m telescope. Adaptive optics spectroscopy with the integral field spectrograph OSIRIS on the Keck 10 m telescope reveals that the companion has a spectral type of M8 ± 1. According to substellar evolution models, the M8 spectral type resides within the substellar mass regime at the age of the Pleiades. The primary itself is a known double-lined spectroscopic binary, which makes the resolved companion, H ii 1348B, the least massive and widest component of this hierarchical triple system and the first substellar companion to a stellar primary in the Pleiades.

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OSIRIS: A diffraction limited integral field spectrograph for Keck

Cited by 127 publications

References 1 publication

The Nature of Active Galactic Nuclei With Velocity Offset Emission Lines*

The Nature of Active Galactic Nuclei With Velocity Offset Emission Lines*

A Normal Supermassive Black Hole in Ngc 1277

A Substellar Common Proper-Motion Companion to the Pleiad H Ii 1348

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