SITELLE: an Imaging Fourier Transform Spectrometer for the Canada–France–Hawaii Telescope

Drissen, Laurent; Martin, Thomas; Rousseau-Nepton, Laurie; Robert, Carmelle; Martin, R. P.; Baril, Marc; Prunet, S.; Joncas, G.; Thibault, Simon; Brousseau, Denis; Mandar, Julie; Grandmont, Frédéric; Yee, H. K. C.; Simard, Luc

doi:10.1093/mnras/stz627

Cited by 51 publications

(42 citation statements)

References 33 publications

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“…The ILS function for SITELLE is a pure cardinal sine (sinc) function. The FWHM of the sinc function is known and fixed since it depends only on the sampling and the maximum optical path displacement of the interferogram scan (Martin et al 2016;Drissen et al 2019). As shown in the work of Martin et al (2016), when natural line broadening is observed, a sinc convolved with a Gaussian function can be used to properly recover the line parameters.…”

Section: Data Reduction and Calibrationsmentioning

confidence: 99%

“…Multiple instruments (i.e. Integral Field Spectrographs ; IFS, Imaging Fourier Transform Spectrograph ; IFTS, and Fabry-Perot) have been implemented for this purpose in the visible/near-infrared, most notably the Spectroscopic Areal Unit for Research on Optical Nebulae (SAURON, Bacon et al 2001), Fabry-Perot instruments at the Observatoire de Haute-Provence (Garrido et al 2002) and the Observatoire du Mont-Mégantic (Hernandez et al 2003), the Infrared Spectrograph on the Spitzer Space Telescope (IRS, Houck et al 2004), the Potsdam Multi-Aperture Spectrophotometer -fiber Package (PMAS-PPAK, Roth et al 2005), the Visible Integral-Field Replicable Unit Spectrographs prototype (VIRUS-P, Hill et al 2008), the Multi Unit Spectroscopic Explorer (MUSE, Laurent et al 2006;Bacon et al 2010), the Sydney-AAO Multi-object Integral Field Spectrograph (SAMI, Bryant et al 2012), the Sloan Digital Sky Survey IV (SDSS-IV, Drory et al 2015), and the Spectro-Imageurà Transformée de Fourier pour l'Étude en Long et en Large des raies d'Émission (SITELLE, Brousseau et al 2014;Drissen et al 2019). Many other instruments with integral-field capabilities are currently being developed, e.g.…”

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confidence: 99%

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SIGNALS: I. Survey description

Rousseau-Nepton

Martin

Robert

et al. 2019

Monthly Notices of the Royal Astronomical Society

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SIGNALS, the Star formation, Ionized Gas, and Nebular Abundances Legacy Survey, is a large observing program designed to investigate massive star formation and H II regions in a sample of local extended galaxies. The program will use the imaging Fourier transform spectrograph SITELLE at the Canada-France-Hawaii Telescope. Over 355 hours (54.7 nights) have been allocated beginning in fall 2018 for eight consecutive semesters. Once completed, SIGNALS will provide a statistically reliable laboratory to investigate massive star formation, including over 50 000 resolved H II regions : the largest, most complete, and homogeneous database of spectroscopically and spatially resolved extragalactic H II regions ever assembled. For each field observed, three datacubes covering the spectral bands of the filters SN1 (363 -386 nm), SN2 (482 -513 nm), and SN3 (647 -685 nm) are gathered. The spectral resolution selected for each spectral band is 1000, 1000, and 5000, respectively. As defined, the project sample will facilitate the study of small-scale nebular physics and many other phenomena linked to star formation at a mean spatial resolution of ∼20 pc. This survey also has considerable legacy value for additional topics including planetary nebulae, diffuse ionized gas, and supernova remnants. The purpose of this paper is to present a general outlook of the survey, notably the observing strategy, galaxy sample, and science requirements.

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Section: Data Reduction and Calibrationsmentioning

confidence: 99%

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confidence: 99%

SIGNALS: I. Survey description

Rousseau-Nepton

Martin

Robert

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…NGC 3344 was observed in March 2016 (RUNID: 16AH41; PI: R.P. Martin) with the imaging Fourier transform spectrometer (iFTS) SITELLE (Drissen et al 2010(Drissen et al , 2019 installed on the 3.6-m Canada-France-Hawaii Telescope (CFHT). With a large 11 × 11 field of view (FoV) and a seeinglimited spatial resolution sampled at 0.32 , SITELLE allows us to obtain more than 4 million spectra in the wavelength range from 350 to 900 nm.…”

Section: Observationmentioning

confidence: 99%

“…ORBS is an automatic data reduction software designed for iFTS data obtained with SITELLE freely available on the web 2 . ORBS follows in a few steps to transform the interferogram cubes (from the two cameras) into a spectral datacube for each filter (see Drissen et al 2019). First, the standard CCD image calibrations are applied, including the bias subtraction, the flat-field correction, and the cosmic rays removal.…”

Section: Data Reduction and Lines Fittingmentioning

confidence: 99%

3D optical spectroscopic study of NGC 3344 with SITELLE: I. Identification and confirmation of supernova remnants

Moumen

Robert

Devost

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present the first optical identification and confirmation of a sample of supernova remnants (SNRs) in the nearby galaxy NGC 3344. Using high spectral and spatial resolution data, obtained with the CFHT imaging Fourier transform spectrograph SITELLE, we identified about 2200 emission line regions, many of which are H II regions, diffuse ionized gas regions, and also SNRs. Considering the stellar population and diffuse ionized gas background, that are quite important in NGC 3344, we have selected 129 SNR candidates based on four criteria for regions where the emission lines flux ratio [S II]/Hα ≥ 0.4. Emission lines of [O II]λ3727, Hβ, [O III]λλ4959,5007, Hα, [N II]λλ6548,6583, and [S II]λλ6716,6731 have been measured to study the ionized gas properties of the SNR candidates. We adopted a self-consistent spectroscopic analysis, based on Sabbadin plots and BPT diagrams, to confirm the shock-heated nature of the ionization mechanism in the candidates sample. With this analysis, we end up with 42 Confirmed SNRs, 45 Probable SNRs, and 42 Less likely SNRs. Using shock models, the Confirmed SNRs seems to have a metallicity ranging between LMC and 2×solar. We looked for correlations between the size of the Confirmed SNRs and their emission lines ratios, their galaxy environment, and their galactocentric distance: we see a trend for a metallicity gradient among the SNR population, along with some evolutionary effects.

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“…The data presented here consist of three multispectral data cubes obtained with the optical imaging Fourier Transform Spectrometer (iFTS), SITELLE, attached to the 3.6-meter Canada-France-Hawaii Telescope (Drissen et al 2019). SITELLE delivers multispectral cubes covering a 11 ×11 field-of-view, sampled with 0.32 pixels, covering specific bandpasses of the visible band using filters .…”

Section: Observationsmentioning

confidence: 99%

A multispectral analysis of the northeastern shell of IC 443

Alarie

Drissen

2019

Monthly Notices of the Royal Astronomical Society

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We have carried out optical observations of the north-eastern part of the supernova remnant IC 443 using the CFHT imaging spectrograph SITELLE. The observations consist of three multispectral cubes covering an 11 ×11 area allowing the investigation of both the spatial and spectral variation of 9 emission lines : [O II] λ λ 3726+3729, [O III] λ λ 4959,5007, Hβ , Hα, [N II] λ λ 6548,6583 and [S II] λ λ 6716,6731. Extinction measurement from the Hα/ Hβ shows significant variation across the observed region with E(B-V) = 0.8-1.1. Electron density measurements using [S II] lines indicate densities ranging from 100 up to 2500 cm −3 . Models computed with the shock modelling code MAPPINGS are presented and compared with the observations. A combination of complete shock model and truncated ones are required in order to explain the observed spectrum. The shock velocities found in IC 443 are between 20 and 150 km s −1 with 75 km s −1 being the most prominent velocity. The pre-shock number density varies from 20 to 60 cm −3 . A single set of abundances close to solar values combined with varying shock parameters (shock velocity, pre-shock density and shock age) are sufficient to explain to great variation of lines intensities observed in IC 443. Despite the relatively modest spectral resolution of the data (R∼ 1500 at Hα), we clearly separate the red and blue velocity components of the expanding nebula, which show significant morphological differences.

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SITELLE: an Imaging Fourier Transform Spectrometer for the Canada–France–Hawaii Telescope

Cited by 51 publications

References 33 publications

SIGNALS: I. Survey description

SIGNALS: I. Survey description

3D optical spectroscopic study of NGC 3344 with SITELLE: I. Identification and confirmation of supernova remnants

A multispectral analysis of the northeastern shell of IC 443

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