Comparing the Locations of Supernovae to CO (2–1) Emission in Their Host Galaxies

Chen, Ness Mayker; Leroy, Adam K.; Lopez, Laura A.; Benincasa, Samantha M.; Chevance, Mélanie; Glover, Simon C. O.; Hughes, Annie; Kreckel, Kathryn; Sarbadhicary, Sumit K.; Sun, Jiayi; Thompson, Todd A.; Utomo, Dyas; Bigiel, Frank; Blanc, Guillermo A.; Dale, Daniel A.; Grasha, Kathryn; Kruijssen, J. M. Diederik; Pan, Hsi-An; Schinnerer, E.; Watkins, Elizabeth J.; Williams, Thomas G.

doi:10.3847/1538-4357/acab00

Cited by 4 publications

(2 citation statements)

References 127 publications

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“…Here we primarily focus on the detection of CO emission, reporting if there is significant (signal-to-noise >3) CO (2-1) emission present. For a more detailed analysis of CO (2-1) emission at the sites of SNe explosions in the PHANGS galaxies, with more description of how we handle the PHANGS-ALMA CO (2-1) data, see Mayker Chen et al (2023).…”

Section: Datamentioning

confidence: 99%

“…We took the first step toward this goal of characterizing the local sites of SNe in Mayker Chen et al (2023), where we studied the CO (2-1) emission from SNe in the PHANGS-Atacama Large Millimeter/submillimeter Array (ALMA) survey (Leroy et al 2021). In this paper, we take the next logical step: comparing SNe to tracers of the ionized gas and young, massive stars using the PHANGS-Multi-Unit Spectroscopic Explorer (MUSE) survey (Emsellem et al 2022) and including a first look based on the PHANGS-Hα Hubble Space Telescope (HST) survey (P.I.…”

Section: Introductionmentioning

confidence: 99%

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Hα Emission and H ii Regions at the Locations of Recent Supernovae in Nearby Galaxies

Mayker Chen,

Leroy,

Sarbadhicary

et al. 2024

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We present a statistical analysis of the local, ≈50–100 pc scale, Hα emission at the locations of recent (≤125 yr) supernovae (SNe) in nearby star-forming galaxies. Our sample consists of 32 SNe in 10 galaxies that are targets of the PHANGS-MUSE survey. We find that 41% (13/32) of these SNe occur coincident with a previously identified H ii region. For comparison, H ii regions cover 32% of the area within ±1 kpc of any recent SN. Contrasting this local covering fraction with the fraction of SNe coincident with H ii regions, we find a statistical excess of 7.6% ± 8.7% of all SNe to be associated with H ii regions. This increases to an excess of 19.2% ± 10.4% when considering only core-collapse SNe (CCSNe). These estimates appear to be in good agreement with qualitative results from new, higher-resolution Hubble Space Telescope Hα imaging, which also suggests many CCSNe detonate near but not in H ii regions. Our results appear consistent with the expectation that only a modest fraction of stars explode during the first ≲5 Myr of the life of a stellar population when Hα emission is expected to be bright. Of the H ii region associated SNe, 85% (11/13) also have associated detected CO (2–1) emission, indicating the presence of molecular gas. The SNe associated with H ii regions have typical extinctions of A V ∼ 1 mag, consistent with a significant amount of pre-clearing of gas from the region before the SNe explode.

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Section: Datamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Hα Emission and H ii Regions at the Locations of Recent Supernovae in Nearby Galaxies

Mayker Chen,

Leroy,

Sarbadhicary

et al. 2024

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Origin of the diffuse 4–8 keV emission in M 82

Iwasawa¹,

C.²,

Gilli³

et al. 2023

A&A

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We present the first spatially resolved, X-ray spectroscopic study of the 4−8 keV diffuse emission found in the central part of the nearby starburst galaxy M 82 on a few arcsecond scales. The new details that we see allow a number of important conclusions to be drawn on the nature of the hot gas and its origin as well as feedback on the interstellar medium. We use archival data from the Chandra X-ray Observatory with an exposure time of 570 ks. The Fe XXV emission at 6.7 keV, expected from metal-enriched hot gas, is enhanced only in a limited area close to the starburst disc and is weak or almost absent over the rest of the diffuse emission, resulting in spatial variations in equivalent width from < 0.1 keV to 1.9 keV. This shows the presence of non-thermal emission due to inverse Compton scattering of the far-infrared photons by radio emitting cosmic ray electrons. The morphological resemblance between the diffuse X-ray, radio, and far-infrared emission maps support this concept. Our decomposition of the diffuse emission spectrum indicates that ∼70% of the 4−8 keV luminosity originates from the inverse Compton emission. The metal-rich hot gas with a temperature of ≃5 keV makes a minor contribution to the 4−8 keV continuum, but it accounts for the majority of the observed Fe XXV line. This hot gas appears to emerge from the circumnuclear starburst ring and fill the galactic chimneys identified as mid-infrared and radio emission voids. The energetics argument suggests that much of the supernova energy in the starburst site has gone into creating of the chimneys and is transported to the halo. We argue that a hot, rarefied environment produced by strong supernova feedback results in displacing the brightest X-ray and radio supernova remnants which are instead found to reside in giant molecular clouds. We find a faint X-ray source with a radio counterpart, close to the kinematic centre of the galaxy and we carefully examine the possibility that this source is a low-luminosity active galactic nucleus in an advection-dominated accretion flow phase.

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A characterization of ASAS-SN core-collapse supernova environments with VLT+MUSE

Pessi¹,

Prieto²,

Anderson³

et al. 2023

A&A

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Context. The analysis of core-collapse supernova (CCSN) environments can provide important information on the life cycle of massive stars and constrain the progenitor properties of these powerful explosions. The MUSE instrument at the Very Large Telescope (VLT) enables detailed local environment constraints of the progenitors of large samples of CCSNe. Using a homogeneous SN sample from the All-Sky Automated Survey for Supernovae (ASAS-SN) survey, an untargeted and spectroscopically complete transient survey, has enabled us to perform a minimally biased statistical analysis of CCSN environments. Aims. We analyze 111 galaxies observed by MUSE that hosted 112 CCSNe – 78 II, nine IIn, seven IIb, four Ic, seven Ib, three Ibn, two Ic-BL, one ambiguous Ibc, and one superluminous SN – detected or discovered by the ASAS-SN survey between 2014 and 2018. The majority of the galaxies were observed by the All-weather MUse Supernova Integral field Nearby Galaxies (AMUSING) survey. Here we analyze the immediate environment around the SN locations and compare the properties between the different CCSN types and their light curves. Methods. We used stellar population synthesis and spectral fitting techniques to derive physical parameters for all H II regions detected within each galaxy, including the star formation rate (SFR), Hα equivalent width (EW), oxygen abundance, and extinction. Results. We found that stripped-envelope supernovae (SESNe) occur in environments with a higher median SFR, Hα EW, and oxygen abundances than SNe II and SNe IIn/Ibn. Most of the distributions have no statistically significant differences, except between oxygen abundance distributions of SESNe and SNe II, and between Hα EW distributions of SESNe and SNe II. The distributions of SNe II and IIn are very similar, indicating that these events explode in similar environments. For the SESNe, SNe Ic have higher median SFRs, Hα EWs, and oxygen abundances than SNe Ib. SNe IIb have environments with similar SFRs and Hα EWs to SNe Ib, and similar oxygen abundances to SNe Ic. We also show that the postmaximum decline rate, s, of SNe II correlates with the Hα EW, and that the luminosity and the Δm15 parameter of SESNe correlate with the oxygen abundance, Hα EW, and SFR at their environments. This suggests a connection between the explosion mechanisms of these events to their environment properties.

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Comparing the Locations of Supernovae to CO (2–1) Emission in Their Host Galaxies

Cited by 4 publications

References 127 publications

Hα Emission and H ii Regions at the Locations of Recent Supernovae in Nearby Galaxies

Hα Emission and H ii Regions at the Locations of Recent Supernovae in Nearby Galaxies

Origin of the diffuse 4–8 keV emission in M 82

A characterization of ASAS-SN core-collapse supernova environments with VLT+MUSE

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