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

Moumen, Ismael; Robert, Carmelle; Devost, D.; Martin, R. P.; Rousseau-Nepton, Laurie; Drissen, Laurent; Martin, Thomas

doi:10.1093/mnras/stz1734

Cited by 16 publications

(14 citation statements)

References 83 publications

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“…10). To confirm whether this heart-shaped ring in KK 203 is an SNR, one would need to use the emission line ratios as diagnostics (Moumen et al 2019), for which our current observations are too shallow. Moreover, given the low metallicity of the system, it is unclear whether deeper observations could be able to detect other gas emission lines beyond the Balmer series of atomic hydrogen.…”

Section: Continuum Hbeta Oiiimentioning

confidence: 98%

The properties of dwarf spheroidal galaxies in the Cen A group

Müller

Fahrion

Rejkuba

et al. 2021

A&A

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Dwarf spheroidal galaxies (dSphs) have been extensively investigated in the Local Group, but their low luminosity and surface brightness make similar work in more distant galaxy groups challenging. Modern instrumentation unlocks the possibility of scrutinizing these faint systems in other environments, expanding the parameter space of group properties. We use MUSE spectroscopy to study the properties of 14 known or suspected dSph satellites of Cen A. Twelve targets are confirmed to be group members based on their radial velocities. Two targets are background galaxies at ∼50 Mpc: KK 198 is a face-on spiral galaxy, and dw1315-45 is an ultradiffuse galaxy with an effective radius of ∼2300 pc. The 12 confirmed dSph members of the Cen A group have old and metal-poor stellar populations and follow the stellar metallicity-luminosity relation defined by the dwarf galaxies in the Local Group. In the three brightest dwarf galaxies (KK 197, KKs 55, and KKs 58), we identify globular clusters, as well as a planetary nebula in KK 197, although its association with this galaxy and/or the extended halo of Cen A is uncertain. Using four discrete tracers, we measure the velocity dispersion and dynamical mass of KK 197. This dSph appears dark matter dominated and lies on the radial acceleration relation of star-forming galaxies within the uncertainties. It also is consistent with predictions stemming from modified Newtonian dynamics (MOND). Surprisingly, in the dwarf KK 203 we find an extended Hα ring. Careful examination of Hubble Space Telescope photometry reveals a very low level of star formation at ages between 30-300 Myr. The Hα emission is most likely linked to a ∼40 Myr old supernova remnant, although other possibilities for its origin cannot be entirely ruled out.

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Section: Continuum Hbeta Oiiimentioning

confidence: 98%

The properties of dwarf spheroidal galaxies in the Cen A group

Müller

Fahrion

Rejkuba

et al. 2021

A&A

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“…SITELLE's narrow SN3 filter precludes this study from the data in-hand, but observations with its SN1 and SN2 filters would afford line ratio measurements to carry out such an investigation (e.g. Rousseau-Nepton et al 2018;Moumen et al 2019;Flagey et al 2020). But in this work, we have not found direct evidence for late accretion in the HIghMass galaxies examined.…”

Section: Radial Flows and Late Accretionmentioning

confidence: 73%

Non-circular flows in HIghMass galaxies in a test of the late accretion hypothesis

Bisaria,

Spekkens,

Huang

et al. 2021

Preprint

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We present Hα velocity maps for the HIghMass galaxies UGC 7899, UGC 8475, UGC 9037 and UGC 9334, obtained with the SITELLE Imaging Fourier Transform Spectrometer on the Canada-France-Hawaii Telescope, to search for kinematic signatures of late gas accretion to explain their large atomic gas reservoirs. The maps for UGC 7899, UGC 9037, and UGC 9334 are amenable to disc-wide radial flow searches with the DiskFit algorithm, and those for UGC 7899 and UGC 9037 are also amenable to inner-disk kinematic analyses. We find no evidence for outer disc radial flows down to Vr ∼ 20 km s −1 in UGC 9037 and UGC 9334, but hints of such flows in UGC 7899. Conversely, we find clear signatures of inner (r 5 kpc) non-circularities in UGC 7899 and UGC 9037 that can be modelled as either bisymmetric (which could be produced by a bar) or radial flows. Comparing these models to the structure implied by photometric disc-bulge-bar decompositions, we favour inner radial flows in UGC 7899 and an inner bar in UGC 9037. With hints of outer disc radial flows and an outer disc warp, UGC 7899 is the best candidate for late accretion among the galaxies examined, but additional modelling is required to disentangle potential degeneracies between these signatures in H I and Hα velocity maps. Our search provides only weak constraints on hot-mode accretion models that could explain the unusually high H I content of HIghMass galaxies.

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“…For the galaxies observed in SI-GNALS, the stellar population continuum subtraction will be performed in three steps: 1) a fit of the gas emission will be performed to obtain an estimate of the velocity field, the emission line fluxes, and the continuum level, 2) the aperture for the stellar continuum sample will be defined using the galaxy luminosity profile, 3) the stellar population spectra will be extracted or fitted through the apertures and used to subtract the component from each spaxel (e.g. Moumen et al 2019). Ideally, when the SNR and spatial resolution allow it, the local environment will be used to build the galaxy background spectrum directly from the datacubes.…”

Section: Stellar Continuum Subtractionmentioning

confidence: 99%

“…Also, the DIG can be observed near H II region boundaries. Recent works on the DIG have helped to quantify its emission in nearby galaxies (Lacerda et al 2018;Poetrodjojo et al 2019;Moumen et al 2019) and photoionization models have been developed to trace back the spectral energy distribution of the source of ionization. Several sources of ionization might be responsible for the DIG : ionizing photons escaping H II regions that travel long distances (Ferguson et al 1996;Haffner et al 2009;Zurita et al 2000;Oey et al 2007;Barnes et al 2014;Howard et al 2016Howard et al , 2017, a weak AGN (Ho 2008;Davies et al 2014), a generation of post-AGB stars (Binette et al 1994;Flores-Fajardo et al 2011 2018), using circular regions only, along with simulations from CLOUDY using post-processing of evolutionary tracks from the WARP-FIELD code Pellegrini et al 2019).…”

Section: Feedback Processesmentioning

confidence: 99%

“…The rich SIGNALS dataset will be valuable for investigating other complementary astrophysical topics. Some possibilities include: 1) planetary nebula abundance distributions and luminosity functions (Kreckel et al 2017;Martin et al 2018); 2) supernova remnant ionization conditions, occurrence, and feedback contribution (Moumen et al 2019); 3) detection of background emission line objects (e.g. [O II] and Ly-α emitters); and 4) large-scale velocity mapping of galaxies.…”

Section: Legacy Valuementioning

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

Cited by 16 publications

References 83 publications

The properties of dwarf spheroidal galaxies in the Cen A group

The properties of dwarf spheroidal galaxies in the Cen A group

Non-circular flows in HIghMass galaxies in a test of the late accretion hypothesis

SIGNALS: I. Survey description

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