Detection of supernova remnants in NGC 4030

Fernandes, R. Cid; Carvalho, M. S.; Sánchez, S. F.; Amorim, A.; Ruschel-Dutra, D.

doi:10.1093/mnras/stab059

Cited by 14 publications

(5 citation statements)

References 56 publications

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“…They selected the SNRs candidates using a combination of criteria: [S ii]λλ6717, 6731/Hα > 0.4, high S/N for the two [S ii]λλ6717, 6731 lines, size of the region < 120 pc and finally they require concentrated regions based on their pseudo-Voight profile. Finally, Cid Fernandes et al (2021) (Green 2019), most of which have been identified through their radio emission. If we consider only the BPT sub-sample, which should contain only the most reliable detections, we detect ∼ 100 SNRs per galaxy on average, still on the same order of magnitude as what is found in the literature.…”

Section: Planetary Nebulae Luminosity Functionmentioning

confidence: 99%

PHANGS-MUSE: Detection and Bayesian classification of ~40 000 ionised nebulae in nearby spiral galaxies

Congiu

Blanc

Belfiore

et al. 2023

A&A

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In this work, we present a new catalogue of > 40000 ionised nebulae distributed across the 19 galaxies observed by the PHANGS-MUSE survey. The nebulae have been classified using a new model-comparison-based algorithm that exploits the odds ratio principle to assign a probabilistic classification to each nebula in the sample. The resulting catalogue is the largest catalogue containing complete spectral and spatial information for a variety of ionised nebulae available so far in the literature. We developed this new algorithm to address some of the main limitations of the traditional classification criteria, such as their binarity, the sharpness of the involved limits, and the limited amount of data they rely on for the classification. The analysis of the catalogue shows that the algorithm performs well when selecting H ii regions. In fact, we can recover their luminosity function, and its properties are in line with what is available in the literature. We also identify a rather significant population of shock-ionised regions (mostly composed of supernova remnants), which is an order of magnitude larger than any other homogeneous catalogue of supernova remnants currently available in the literature. The number of supernova remnants we identify per galaxy is in line with results in our Galaxy and in other very nearby sources. However, limitations in the source detection algorithm result in an incomplete sample of planetary nebulae, even though their classification seems robust. Finally, we demonstrate how applying a correction for the contribution of the diffuse ionised gas to the nebulae's spectra is essential to obtain a robust classification of the objects and how a correct measurement of the extinction using diffuse-ionised-gas-corrected line fluxes prompts the use of a higher theoretical Hα/Hβ ratio (3.03) than what is commonly used when recovering the E(B − V) via the Balmer decrement technique in massive star-forming galaxies.

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Section: Planetary Nebulae Luminosity Functionmentioning

confidence: 99%

PHANGS-MUSE: Detection and Bayesian classification of ~40 000 ionised nebulae in nearby spiral galaxies

Congiu

Blanc

Belfiore

et al. 2023

A&A

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“…This is the reason why this parameter is used to discriminate the ionizing source in the WHAN diagram (panel c). In this particular galaxy we find anomalous large values of the N2 ratio compared to those at the same galactocentric distances at the location of the reported SNR (e.g., Cid Fernandes et al 2021). We stress that this N2-enhancement is a direct consequence of an extra ionizing source, and should never be considered as an increase of the oxygen abundance.…”

Section: Ngc 2906: Resolved Properties Of the Ionized Gasmentioning

confidence: 49%

The Calar Alto Legacy Integral Field Area Survey: Spatial Resolved Properties

Sánchez,

Barrera-Ballesteros,

Galbany

et al. 2024

RMxAA

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We present the analysis using the pyPipe3D pipeline for the 895 galaxies that comprises the eCALIFA data release (Sanchez et al. 2023), data with a significantly improved spatial resolution (1.0-1.5''/FWHM). We include a description of (i) the analysis performed by the pipeline, (ii) the adopted datamodel for the derived spatially resolved properties and (iii) the catalog of integrated, characteristics and slope of the radial gradients for a set of observational and physical parameters derived for each galaxy. We illustrate the results of the analysis (i) using the NGC 2906 galaxy, showing the spatial distribution of the different derived parameters, and (ii) showing the distribution of the spatial resolved ionized gas across the [OIII]/Hβ vs. [NII]/Hα diagram for the whole galaxy sample. A general agreement is found with published results, with a clear improvement in the tracing of radial patterns and the segregation of individual ionized structures. Access to all the discussed dataproducts: http://ifs.astroscu.unam.mx/CALIFA_WEB/public_html/.

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“…The [S II] line used in the D16 index may be affected by ionization due to supernova remnants in galaxies, making it susceptible to contamination (e.g., Kopsacheili et al 2020;Cid Fernandes et al 2021). We therefore estimate the occurrence of CCSN per unit of SF, given by Equation (2), using indicators independent of [S II].…”

Section: Discussionmentioning

confidence: 99%

A Metallicity Dependence on the Occurrence of Core-collapse Supernovae

Pessi,

Anderson,

Lyman

et al. 2023

ApJL

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Core-collapse supernovae (CCSNe) are widely accepted to be caused by the explosive death of massive stars with initial masses ≳8 M ⊙. There is, however, a comparatively poor understanding of how properties of the progenitors—mass, metallicity, multiplicity, rotation, etc.—manifest in the resultant CCSN population. Here, we present a minimally biased sample of nearby CCSNe from the All-Sky Automated Survey for Supernovae survey whose host galaxies were observed with integral-field spectroscopy using MUSE at the Very Large Telescope. This data set allows us to analyze the explosion sites of CCSNe within the context of global star formation properties across the host galaxies. We show that the CCSN explosion site oxygen abundance distribution is offset to lower values than the overall H ii region abundance distribution within the host galaxies. We further split the sample at 12 + log 10 ( O / H ) = 8.6 dex and show that within the subsample of low-metallicity host galaxies, the CCSNe unbiasedly trace the star formation with respect to oxygen abundance, while for the subsample of higher-metallicity host galaxies, they preferentially occur in lower-abundance star-forming regions. We estimate the occurrence of CCSNe as a function of oxygen abundance per unit star formation and show that there is a strong decrease as abundance increases. Such a strong and quantified metallicity dependence on CCSN production has not been shown before. Finally, we discuss possible explanations for our result and show that each of these has strong implications not only for our understanding of CCSNe and massive star evolution but also for star formation and galaxy evolution.

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Detection of supernova remnants in NGC 4030

Cited by 14 publications

References 56 publications

PHANGS-MUSE: Detection and Bayesian classification of ~40 000 ionised nebulae in nearby spiral galaxies

PHANGS-MUSE: Detection and Bayesian classification of ~40 000 ionised nebulae in nearby spiral galaxies

The Calar Alto Legacy Integral Field Area Survey: Spatial Resolved Properties

A Metallicity Dependence on the Occurrence of Core-collapse Supernovae

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