The Gemini Near‐Infrared Imager (NIRI)

Hodapp, Klaus W.; Jensen, Joseph B.; Irwin, Everett M.; Yamada, Haruka; Chung, Randolph; Fletcher, Kent; Robertson, Louis; Hora, J. L.; Simons, Douglas A.; Mays, Wendy; Nolan, Robert; Bec, Matthieu; Merrill, Michael; Fowler, Albert M.

doi:10.1086/379669

Cited by 285 publications

(235 citation statements)

References 21 publications

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“…NIRI (Hodapp et al 2003) is installed at the Gemini North telescope in Hawaii. It was used in combination with the ALTAIR AO system (Herriot et al 2000) to obtain diffractionlimited images on a 1024 × 1024 Aladdin InSb detector array.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

The International Deep Planet Survey

Vigan

Patience

Marois

et al. 2012

A&A

155

200

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Breakthrough direct detections of planetary companions orbiting A-type stars confirm the existence of massive planets at relatively large separations, but dedicated surveys are required to estimate the frequency of similar planetary systems. To measure the first estimation of the giant exoplanetary systems frequency at large orbital separation around A-stars, we have conducted a deep-imaging survey of young (8−400 Myr), nearby (19−84 pc) A-and F-stars to search for substellar companions in the ∼10−300 AU range. The sample of 42 stars combines all A-stars observed in previous AO planet search surveys reported in the literature with new AO observations from VLT/NaCo and Gemini/NIRI. It represents an initial subset of the International Deep Planet Survey (IDPS) sample of stars covering M-to B-stars. The data were obtained with diffraction-limited observations in H-and K s -band combined with angular differential imaging to suppress the speckle noise of the central stars, resulting in typical 5σ detection limits in magnitude difference of 12 mag at 1 , 14 mag at 2 and 16 mag at 5 which is sufficient to detect massive planets. A detailed statistical analysis of the survey results is performed using Monte Carlo simulations. Considering the planet detections, we estimate the fraction of A-stars having at least one massive planet (3−14 M Jup ) in the range 5−320 AU to be inside 5.9−18.8% at 68% confidence, assuming a flat distribution for the mass of the planets. By comparison, the brown dwarf (15−75 M Jup ) frequency for the sample is 2.0−8.9% at 68% confidence in the range 5−320 AU. Assuming power law distributions for the mass and semimajor axis of the planet population, the AO data are consistent with a declining number of massive planets with increasing orbital radius which is distinct from the rising slope inferred from radial velocity (RV) surveys around evolved A-stars and suggests that the peak of the massive planet population around A-stars may occur at separations between the ranges probed by existing RV and AO observations. Finally, we report the discovery of three new close M-star companions to HIP 104365 and HIP 42334.

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Section: Observations and Data Reductionmentioning

confidence: 99%

The International Deep Planet Survey

Vigan

Patience

Marois

et al. 2012

A&A

155

200

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“…The field of 4U 0142+61 was imaged in the K s band with the Near Infrared Imager (NIRI; Hodapp et al 2003) on Gemini North, Hawaii, in the night of July 26th, 2005. NIRI has standard broad-band and narrow-band filters covering 1-5 µm.…”

Section: Optical and Nir: Geminimentioning

confidence: 99%

The first multi-wavelength campaign of AXP 4U 0142+61 from radio to hard X-rays

Hartog

Kuiper

Hermsen

et al. 2007

Astrophys Space Sci

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For the first time a quasi-simultaneous multiwavelength campaign has been performed on an Anomalous X-ray Pulsar from the radio to the hard X-ray band. 4U 0142+61 was an INTEGRAL target for 1 Ms in July 2005. During these observations it was also observed in the X-ray band with Swift and RXTE, in the optical and NIR with Gemini North and in the radio with the WSRT. In this paper we present the source-energy distribution. The spectral results obtained in the individual wave bands do not connect smoothly; apparently components of different origin contribute to the total spectrum. Remarkable is that the INTEGRAL hard X-ray spectrum (power-law index 0.79 ± 0.10) is now measured up to an energy of ∼230 keV with no indication of a spectral break. Extrapolation of the INTEGRAL power-law spectrum to lower energies passes orders of magnitude underneath the NIR and optical fluxes,

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“…The facility near-IR imager NIRI (Hodapp et al 2003) was used for the observations with a K-band filter. The total exposure time for the images was 30 s. A small dither sequence was applied keeping the IR object on the image in all spatial positions.…”

Section: Imagingmentioning

confidence: 99%

An outbursting protostar of the FU Orionis type in the Cygnus OB7 molecular cloud

Movsessian¹,

Khanzadyan

Aspin³

et al. 2006

A&A

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Context. To follow the early evolution of stars we need to understand how young stars accrete and eject mass. It is generally assumed that the FU Orionis phenomenon is related to the variations in the disk accretion, but many questions remain still open, in particular because of the rarity of FU Ori type stars. Aims. We explore here the characteristics of the outburst and of the environment of one new object, discovered recently in the active star formation region containing RNO 127, within the Cygnus OB7 dark cloud complex. Methods. We present an extensive optical and near-infrared study of a new candidate of FU Orionis object, including its direct imaging, spectroscopy and scanning Fabry-Pérot interferometry. Results. The source, associated with the variable reflection nebula, underwent prodigious outburst. The "Braid" nebula, which appeared in 2000, as is indicated by its name, consists of two intertwined features, illuminated by the outburst. Subsequent NIR observations revealed the bright source, which was not visible on 2MASS images, and its estimated brightening was more than 4 mag. Optical and infrared spectral data show features, which are necessary for the system to be referred to as a FUor object. The bipolar optical flow directed by the axis of nebula also was found. Various estimates give the November/December 1999 as the most probable date for the eruption.

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The Gemini Near‐Infrared Imager (NIRI)

Cited by 285 publications

References 21 publications

The International Deep Planet Survey

The International Deep Planet Survey

The first multi-wavelength campaign of AXP 4U 0142+61 from radio to hard X-rays

An outbursting protostar of the FU Orionis type in the Cygnus OB7 molecular cloud

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