SITELLE optical design, assembly, and testing

Brousseau, Denis; Thibault, Simon; Fortin-Boivin, Simon; Zhang, Hu; Vallée, Philippe; Auger, Hugues; Drissen, Laurent

doi:10.1117/12.2055214

Cited by 4 publications

(3 citation statements)

References 3 publications

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“…Wild et al 2011). It is possible that with high enough spatial resolution observations, such as those with SITELLE (Brousseau et al 2014;Drissen et al 2019) or SDSS-V Local Volume Mapper (Kollmeier et al 2017), this effect could be measured directly.…”

Section: Warpfield-pop Simulationmentioning

confidence: 99%

Less than the sum of its parts: the dust-corrected H α luminosity of star-forming galaxies explored at different spatial resolutions with MaNGA and MUSE

Asari

Wild

Amorim

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The Hα and Hβ emission line luminosities measured in a single integrated spectrum are affected in non-trivial ways by point-to-point variations in dust attenuation in a galaxy. This work investigates the impact of this variation when estimating global Hα luminosities corrected for the presence of dust by a global Balmer decrement. Analytical arguments show that the dust-corrected Hα luminosity is always underestimated when using the global Hα/Hβ flux ratio to correct for dust attenuation. We measure this effect on 156 face-on star-forming galaxies from the Mapping Nearby Galaxies at APO (MaNGA) survey. At 1–2 kpc spatial resolution, the effect is small but systematic, with the integrated dust-corrected Hα luminosity underestimated by 2–4 per cent (and typically not more than by 10 per cent), and depends on the specific star formation rate of the galaxy. Given the spatial resolution of MaNGA, these are lower limits for the effect. From Multi Unit Spectroscopic Explorer (MUSE) observations of NGC 628 with a resolution of 36 pc we find the discrepancy between the globally and the point-by-point dust-corrected Hα luminosity to be 14 ± 1 per cent, which may still underestimate the true effect. We use toy models and simulations to show that the true difference depends strongly on the spatial variance of the Hα/Hβ flux ratio, and on the slope of the relation between Hα luminosity and dust attenuation within a galaxy. Larger samples of higher spatial resolution observations are required to quantify the dependence of this effect as a function of galaxy properties.

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Section: Warpfield-pop Simulationmentioning

confidence: 99%

Less than the sum of its parts: the dust-corrected H α luminosity of star-forming galaxies explored at different spatial resolutions with MaNGA and MUSE

Asari

Wild

Amorim

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Details about SITELLE's optical design, assembly, and testing are provided by Brousseau et al (2014), so we only present here a brief overview. SITELLE's optics consists of two groups: a collimator with a focal length of 711.3 mm, composed of three lenses and two identical cameras with a focal length of 236.3 mm, which contain six lenses each.…”

Section: Optical Designmentioning

confidence: 99%

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

Drissen

Martin

Rousseau-Nepton

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present an overview of SITELLE, an Imaging Fourier Transform Spectrometer (iFTS) available at the 3.6-meter Canada-France-Hawaii Telescope. SITELLE is a Michelson-type interferometer able to reconstruct the spectrum of every light source within its 11 field of view in filter-selected bands of the visible (350 to 900 nm). The spectral resolution can be adjusted up to R = 10 000 and the spatial resolution is seeinglimited and sampled at 0.32 per pixel. We describe the design of the instrument as well as the data reduction and analysis process. To illustrate SITELLE's capabilities, we present some of the data obtained during and since the August 2015 commissioning run. In particular, we demonstrate its ability to separate the components of the [OII] λλ 3726,29 doublet in Orion and to reach R = 9500 around Hα; to detect diffuse emission at a level of 4 × 10 −17 erg cm −2 s −1 arcsec −2 ; to obtain integrated spectra of stellar absorption lines in galaxies despite the well-known multiplex disadvantage of the iFTS; and to detect emission-line galaxies at different redshifts.

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“…In order to obtain the desired spectral resolution in a reasonable amount of time while reducing the background photon noise, filters are inserted in the optical path. More details about SITELLE, its metrology system and its performances, are given in Grandmont et al (2012); Drissen et al (2014); Brousseau et al (2014); Drissen et al (2016).…”

Section: Description Of the Instrumentmentioning

confidence: 99%

When does an old nova become a dwarf nova? Kinematics and age of the nova shell of the dwarf nova AT Cnc

Shara,

Drissen,

Martin

et al. 2016

Preprint

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The Z Cam-type dwarf nova AT Cnc displays a classical nova (CN) shell, demonstrating that mass transfer in cataclysmic binaries decreases substantially after a CN eruption. The hibernation scenario of cataclysmic binaries predicts such a decrease, on a timescale of a few centuries. In order to measure the time since AT Cnc's last CN eruption, we have measured the radial velocities of a hundred clumps in its ejecta with SITELLE, CFHT's recently commissioned imaging Fourier transform spectrometer. These range from -455 to +490 km/s. Coupled with the known distance to AT Cnc of 460 pc (Shara 2012), the size of AT Cnc's shell, and a simple model of nova ejecta deceleration, we determine that the last CN eruption of this system occurred 330 +135 −90 years ago. This is the most rapid transition from a high mass transfer rate, novalike variable to a low mass transfer rate, dwarf nova yet measured, and in accord with the hibernation scenario of cataclysmic binaries. We conclude by noting the similarity in deduced outburst date (within a century of 1686 CE) of AT Cnc with a "guest star" reported in the constellation Cancer by Korean observers in 1645 CE.

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SITELLE optical design, assembly, and testing

Cited by 4 publications

References 3 publications

Less than the sum of its parts: the dust-corrected H α luminosity of star-forming galaxies explored at different spatial resolutions with MaNGA and MUSE

Less than the sum of its parts: the dust-corrected H α luminosity of star-forming galaxies explored at different spatial resolutions with MaNGA and MUSE

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

When does an old nova become a dwarf nova? Kinematics and age of the nova shell of the dwarf nova AT Cnc

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