A Near-Infrared Adaptive Optics Imaging Survey of Nearby QSOs

2005 ◽  
pp. 338-344
Author(s):  
Olivier Guyon ◽  
Dave Sanders ◽  
Alan Stockton
Keyword(s):  
Adaptive Optics ◽  
Near Infrared ◽  
Adaptive Optics Imaging

scholarly journals Near‐Infrared Adaptive Optics Imaging of High‐Redshift Quasars

2008 ◽  
Vol 673 (2) ◽  
pp. 694-702 ◽  
Author(s):  
Renato Falomo ◽  
Aldo Treves ◽  
Jari K. Kotilainen ◽  
Riccardo Scarpa ◽  
Michela Uslenghi
Keyword(s):  
Adaptive Optics ◽  
Near Infrared ◽  
High Redshift ◽  
Adaptive Optics Imaging

scholarly journals CATS: OPTICAL TO NEAR-INFRARED COLORS OF THE BULGE AND DISK OF TWOz= 0.7 GALAXIES USINGHUBBLE SPACE TELESCOPEAND KECK LASER ADAPTIVE OPTICS IMAGING

2008 ◽  
Vol 136 (4) ◽  
pp. 1523-1532 ◽  
Author(s):  
E. Steinbring ◽  
J. Melbourne ◽  
A. J. Metevier ◽  
D. C. Koo ◽  
M. R. Chun ◽  
...  
Keyword(s):  
Adaptive Optics ◽  
Near Infrared ◽  
Adaptive Optics Imaging

scholarly journals Near‐Infrared Adaptive Optics Imaging of QSO Host Galaxies

2006 ◽  
Vol 166 (1) ◽  
pp. 89-127 ◽  
Author(s):  
O. Guyon ◽  
D. B. Sanders ◽  
Alan Stockton
Keyword(s):  
Adaptive Optics ◽  
Near Infrared ◽  
Host Galaxies ◽  
Adaptive Optics Imaging

scholarly journals Resolving the Multiplicity of Exoplanet Host Stars in Gemini/NIRI Data

2022 ◽  
Vol 6 (1) ◽  
pp. 8
Author(s):  
Kim Miskovetz ◽  
Trent J. Dupuy ◽  
Jessica Schonhut-Stasik ◽  
Keivan G. Stassun
Keyword(s):  
Adaptive Optics ◽  
Proper Motion ◽  
Near Infrared ◽  
Planetary Systems ◽  
Unit Weight ◽  
Imaging Data ◽  
Infrared Imager ◽  
Adaptive Optics Imaging ◽  
Host Stars

Abstract The majority of stars have one or more stellar companions. As exoplanets continue to be discovered, it is crucial to examine planetary systems to identify their stellar companions. By observing a change in proper motion, companions can be detected by the acceleration they induce on their host stars. We selected 701 stars from the Hipparcos–Gaia Catalog of Accelerations (HGCA) that have existing adaptive optics imaging data gathered with Gemini/Near InfraRed Imager (NIRI). Of these, we examined 21 stars known to host planet candidates and reduced their archival NIRI data with Gemini’s DRAGONS software. We assessed these systems for companions using the NIRI images as well as Renormalized Unit Weight Error values in Gaia and accelerations in the HGCA. We detected three known visible companions and found two more systems with no visible companions but astrometric measurements indicating likely unresolved companions.

scholarly journals Detection and characterization of two VLM binaries: LP 1033-31 and LP 877-72

2020 ◽  
Vol 498 (1) ◽  
pp. 737-749
Author(s):  
Subhajeet Karmakar ◽  
A S Rajpurohit ◽  
F Allard ◽  
D Homeier
Keyword(s):  
Adaptive Optics ◽  
Spectral Type ◽  
Near Infrared ◽  
Binding Energies ◽  
Secondary Component ◽  
Large Telescope ◽  
Very Large Telescope ◽  
Adaptive Optics Imaging ◽  
M Dwarf

ABSTRACT Using the high-resolution near-infrared adaptive optics imaging from the NaCo instrument at the Very Large Telescope, we report the discovery of a new binary companion to the M-dwarf LP 1033-31 and also confirm the binarity of LP 877-72. We have characterized both the stellar systems and estimated the properties of their individual components. We have found that LP 1033-31 AB with the spectral type of M4.5+M4.5 has a projected separation of 6.7 ± 1.3 AU. Whereas with the spectral type of M1+M4, the projected separation of LP 877-72 AB is estimated to be 45.8 ± 0.3 AU. The binary companions of LP 1033-31 AB are found to have similar masses, radii, effective temperatures, and log g with the estimated values of 0.20 ± 0.04 $\rm {M}_{\odot }$, 0.22 ± 0.03 $\rm {R}_{\odot }$, and 3200 K, 5.06 ± 0.04. However, the primary of LP 877-72 AB is found to be twice as massive as the secondary with the derived mass of 0.520 ± 0.006 $\rm {M}_{\odot }$. The radius and log g for the primary of LP 877-72 AB are found to be 1.8 and 0.95 times that of the secondary component with the estimated values of 0.492 ± 0.011 $\rm {R}_{\odot }$ and 4.768 ± 0.005, respectively. With an effective temperature of 3750 ± 15 K, the primary of LP 877-72 AB is also estimated to be ∼400 K hotter than the secondary component. We have also estimated the orbital period of LP 1033-31 and LP 877-72 to be ∼28 and ∼349 yr, respectively. The binding energies for both systems are found to be >1043 erg, which signifies that both systems are stable.

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