&lt;title&gt;CFHT's imaging Fourier transform spectrometer&lt;/title&gt;

Simons, Douglas A.; Clark, Christopher C.; Smith, Suzanne; Kerr, John M.; Massey, Stephen C.; Maillard, J. P.

doi:10.1117/12.176746

Cited by 14 publications

(5 citation statements)

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“…A description of the BEAR instrument is given by Simons et al (1994) and Maillard (1995Maillard ( , 2000. Details of the observing campaigns are given in Raynaud (2003) and Raynaud et al (2004).…”

Section: Observations and Data Processingmentioning

confidence: 99%

Spectro-imaging observations of Jupiter’s 2μm auroral emission. II: Thermospheric winds

Chaufray

Greathouse

Gladstone

et al. 2011

Icarus

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Section: Observations and Data Processingmentioning

confidence: 99%

Spectro-imaging observations of Jupiter’s 2μm auroral emission. II: Thermospheric winds

Chaufray

Greathouse

Gladstone

et al. 2011

Icarus

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“…A detailed description of the properties of BEAR is given by Simons et al (1994) and Maillard (1995) -see Maillard (2000) for an updated review. The instrument BEAR results from the coupling of the CFHT step-scan high resolution facility FTS (Maillard & Michel 1982) with a 256×256 HgCdTe facility camera.…”

Section: Observationsmentioning

confidence: 99%

High resolution near-infrared spectro-imaging of NGC 7027

Cox

Huggins

Maillard

et al. 2002

A&A

116

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Abstract. We present near-infrared spectro-imaging of the young planetary nebula NGC 7027 between 2.10 and 2.20 µm with high spatial (0.5 ) and high spectral (8.7 km s −1 ) resolution. The observations, made using BEAR at the CFHT, reveal the detailed morphology and kinematics of the ionized nebula (in the Brγ line and 16 other atomic lines) and the surrounding molecular envelope (in the 1-0 S(1) line of H2). The observations show that the ionized gas forms an elongated (∼6 × 12 , PA = 32• ), limb-brightened shell with an expansion velocity of 19.5 km s −1 along the line of sight. The shell is composed of numerous small condensations and has nearly parallel sides with flattened ends that are not well matched by a uniform ellipsoidal model. Low level Brγ emission is detected at high red-and blue-shifted velocities (±55 km s −1 ) along a bipolar axis at PA = 60• that deviates significantly from that of the main nebula. The H2 emission is distributed at the periphery of the ionized gas, in a limb-brightened, bi-conical shell (∼10 × 13 , PA = 28• ) with enhanced emission at the equator and complex structure at the ends of the major axis. The H2 emission traces the inner edge of the extended molecular envelope seen in CO, and its distribution and intensity are well matched by model predictions of a high-density (nH ∼ 10 6 −10 5 cm −3 ) photo-dissociation region. The kinematic structure of the H2 emission reveals a remarkable series of lobes and openings in the molecular shell. These features are point symmetric about the center, and the most prominent pair aligns with the high velocity, bipolar emission seen in Brγ. These observations demonstrate recent activity by collimated outflows in NGC 7027, with a multiple, bipolar geometry. The interaction of the outflows with the surrounding envelope has significantly affected the morphology of the developing nebula and its environment, and their presence in this well-studied archetype underscores the general importance of outflows in the early shaping history of planetary nebulae.

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“…In the NIR, a spectrographic variant of the scanning Fourier Transform Spectrometer, using a 2-D IR array, invented by Jean-Pierre Maillard, has been successfully used at the 3.6 m CFHT telescope for more than a decade, including on absorption lines [22]. It is however no longer in operation essentially due to the 'non-standard' complexity of the instrument.…”

Section: 2mentioning

confidence: 99%

Astronomical spectroscopy in the last four decades: survival of the fittest

Monnet

2009

Exp Astron

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Spectroscopic astronomical instrumentation has much evolved in the last 40 years. Long-slit grating spectrographs with a photographic plate as the detector working in the 0.3-1 µm range were prevalent up to the early 1970s. The replacement of photographic plates by two-dimensional digital detectors provided gains in sensitivity of two orders of magnitude and much better photometric and radial velocity precision, and opened the 1 to 25 µm infrared domain. Another gain in speed by up to two orders of magnitude was then obtained through the development of various spectroscopic systems, each optimized for a subset of astronomical objects. This development was underpinned by a number of technological advances, in particular the development of automatic data reduction pipelines using sophisticated algorithms. With ever larger and more complex instrument systems for the present 8-10 m diameter telescopes-and soon even more for the next generation of Extremely Large Telescopes, the development of an instrument is now a big enterprise, ranging all the way from long-term enabling technology efforts to management of large teams for construction and deployment over typically 7-8 years.

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<title>CFHT's imaging Fourier transform spectrometer</title>

Cited by 14 publications

References 0 publications

Spectro-imaging observations of Jupiter’s 2μm auroral emission. II: Thermospheric winds

Spectro-imaging observations of Jupiter’s 2μm auroral emission. II: Thermospheric winds

High resolution near-infrared spectro-imaging of NGC 7027

Astronomical spectroscopy in the last four decades: survival of the fittest

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