Near-identical star formation rate densities from Hα and FUVat redshift zero

Audcent-Ross, Fiona; Meurer, G. R.; Wong, O. I.; Zheng, Zhimin; Hanish, D. J.; Bland-Hawthorn, Joss; Elagali, Ahmed; Meyer, M.; Putman, Mary E.; Ryan-Weber, E. V.; Sweet, Sarah M.; Thilker, David A.; Seibert, Mark; Allen, Ronald J.; Dopita, M. A.; Doyle-Pegg, M. T.; Drinkwater, Michael J.; Ferguson, Harry; Freeman, K. C.; Heckman, Timothy M.; Kennicutt, Robert C.; Kilborn, V. A.; Kim, Ji Hoon; Knezek, P. M.; Koribalski, B. S.; Smith, R. C.; Webster, R. L.; Werk, Jessica K.

doi:10.1093/mnras/sty1538

Cited by 9 publications

(10 citation statements)

References 132 publications

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“…Meurer et al [42] and Audcent-Ross et al [43] pointed out that the burstlike nature of star formation in low-mass galaxies shows up in their average surface brightness. The left-side panel in Fig.…”

Section: Resultsmentioning

confidence: 99%

Star Formation in Nearby Dwarf Galaxies

Кайсин

Караченцев

2019

Astrophys. Bull.

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We report the measured Hα fluxes and images of 66 nearby objects observed with the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences.Three of these objects IC 2233, UGC 4704, and NGC 3432 are late-type spiral galaxies, six objects are distant globular clusters of the M31 galaxy, and the remaining ones are dwarf galaxies. We used the measured Hα fluxes to estimate the integrated and specific starformation rates and analyzed some of the main features of star formation in dwarf galaxies and late-type spirals based on a sample of more than 500 Local-volume galaxies.

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Section: Resultsmentioning

confidence: 99%

Star Formation in Nearby Dwarf Galaxies

Кайсин

Караченцев

2019

Astrophys. Bull.

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“…In order to ease comparisons with previous studies, in this paragraph we adopt the Kroupa IMF results. For fields W1, W2, and W3, the star formation intensity, estimated by MS stars or the UV flux, of ∼10 −4.2 is 2.5 dex weaker than typically found in disc galaxies (as calculated from the H α effective surface brightness corresponding to the median contribution to the volume-averaged H α emissivity of the local Universe as sampled by the SINGG survey Hanish et al 2006;Audcent-Ross et al 2018). Table 7 shows the star formation intensity in the W4 field is about a factor of 10 times even more dilute than the other fields, closer to the radially averaged star formation intensity of the outer disc.…”

Section: Comparison Of Star Formation Intensity Estimatesmentioning

confidence: 86%

The initial mass function in the extended ultraviolet disc of M83

Bruzzese

Thilker

Meurer

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Using Hubble Space Telescope ACS/WFC data we present the photometry and spatial distribution of resolved stellar populations of four fields within the extended ultraviolet disc (XUV disc) of M83. These observations show a clumpy distribution of main-sequence stars and a mostly smooth distribution of red giant branch stars. We constrain the upper end of the initial mass function (IMF) in the outer disc using the detected population of main-sequence stars and an assumed constant star formation rate (SFR) over the last 300 Myr. By comparing the observed main-sequence luminosity function to simulations, we determine the best-fitting IMF to have a power-law slope α = −2.35 ± 0.3 and an upper mass limit $M_{\rm u}=25_{-3}^{+17} \, \mathrm{M}_\odot$. This IMF is consistent with the observed H $\rm \alpha$ emission, which we use to provide additional constraints on the IMF. We explore the influence of deviations from the constant SFR assumption, finding that our IMF conclusions are robust against all but strong recent variations in SFR, but these are excluded by causality arguments. These results, along with our similar studies of other nearby galaxies, indicate that some XUV discs are deficient in high-mass stars compared to a Kroupa IMF. There are over one hundred galaxies within 5 Mpc, many already observed with HST, thus allowing a more comprehensive investigation of the IMF, and how it varies, using the techniques developed here.

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“…The surveys have been used to measure the local star formation rate density, highlighting the importance of the contributions made from galaxy types that can be underrepresented in optically-selected samples: low Hi mass, low luminosity and low surface brightness galaxies (Hanish et al 2006;Audcent-Ross et al 2018). Evidence of possible reduced massive star formation has been detected in low luminosity and low surface brightness galaxies as well as in the outskirts of galaxies (Meurer et al 2009;Bruzzese et al 2015;Watts et al 2018;Bruzzese et al 2019).…”

Section: The Singg and Sungg Surveysmentioning

confidence: 99%

The radial distribution of supernovae compared to star formation tracers

Audcent-Ross

Meurer

Audcent

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Given the limited availability of direct evidence (pre-explosion observations) for supernova (SN) progenitors, the location of supernovae (SNe) within their host galaxies can be used to set limits on one of their most fundamental characteristics, their initial progenitor mass. We present our constraints on SN progenitors derived by comparing the radial distributions of 80 SNe in the SINGG and SUNGG surveys to the R-band, Hα, and UV light distributions of the 55 host galaxies. The strong correlation of Type Ia SNe with R-band light is consistent with models containing only low mass progenitors, reflecting earlier findings. When we limit the analysis of Type II SNe to apertures containing 90 per cent of the total flux, the radial distribution of these SNe best traces far ultraviolet (FUV) emission, consistent with recent direct detections indicating Type II SNe have moderately massive red supergiant progenitors. Stripped Envelope (SE) SNe have the strongest correlation with Hα fluxes, indicative of very massive progenitors (M * 20 M ). This result contradicts a small, but growing, number of direct detections of SE SN progenitors indicating they are moderately massive binary systems. Our result is consistent, however, with a recent population analysis suggesting binary SE SN progenitor masses are regularly underestimated. SE SNe are centralised with respect to Type II SNe and there are no SE SNe recorded beyond half the maximum disc radius in the optical and one third the disc radius in the ultraviolet. The absence of SE SNe beyond these distances is consistent with reduced massive star formation efficiencies in the outskirts of the host galaxies.

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Near-identical star formation rate densities from Hα and FUVat redshift zero

Cited by 9 publications

References 132 publications

Star Formation in Nearby Dwarf Galaxies

Star Formation in Nearby Dwarf Galaxies

The initial mass function in the extended ultraviolet disc of M83

The radial distribution of supernovae compared to star formation tracers

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