Data Aggregation and Unification

Boissier, Daniel; Talon, Aurélie

doi:10.1002/9781118601099.ch9

Cited by 6 publications

(9 citation statements)

References 4 publications

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“…The SFR computed in the inner part of M94 is ∼0.1 M ⊙ yr −1 kpc −2 , and can be deduced from the data in Boissier et al (2007, their fig. 9.39, for H i +H 2 ) and Trujillo et al (2009, for their ‘bulge’ inner region, from FUV data).…”

Section: Age Mapsmentioning

confidence: 63%

Age patterns in a sample of spiral galaxies

Sánchez-Gil

Jones

Pérez

et al. 2011

Monthly Notices of the Royal Astronomical Society

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We present the burst ages for young stellar populations in a sample of six nearby (<10 Mpc) spiral galaxies using a differential pixel‐based analysis of the ionized gas emission. We explore this as an alternative approach for connecting large‐scale dynamical mechanisms with star formation processes in disc galaxies, based on burst ages derived from the Hα to far‐UV (FUV) flux ratio. Images of each galaxy in Hα were taken with Taurus Tunable Filter and matched to FUV imaging from GALEX. The resulting flux ratio provides a robust measure of relative age across the disc which we discuss in terms of the large‐scale dynamical motions. Systematic effects such as a variable initial mass function, non‐solar metallicities, variable star formation histories (SFHs) and dust attenuation have been used to derive estimates of the systematic uncertainty. The resulting age maps show a wide range of patterns outside of those galaxies with the strongest spiral structure, confirming the idea that star formation is driven one by several processes, largely determined by the individual circumstances of the galaxy. Generally, grand design spirals such as M74, M100 and M51 exhibit age gradients across the main spiral arms, with the youngest star formation regions along the central and inner edges. Likewise, in the dominant star‐forming complex of IC 2574 or the ring of M94, the most recent star formation is centrally confined to the regions of star formation activity. In M63 and M74 galaxy‐wide trends emerge, contrary to the spiral structure in these galaxies, suggesting that spiral density waves are not the dominant driver in some cases. We argue that despite appearances, galaxy morphology is not an absolute discriminator of the SFH of an individual galaxy, nor of the processes triggering it. We conclude that Hα‐to‐FUV flux ratios are a relatively direct way to probe burst ages across galaxies and infer something of their dynamical histories, provided that sources of systematics are properly taken into account.

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Section: Age Mapsmentioning

confidence: 63%

Age patterns in a sample of spiral galaxies

Sánchez-Gil

Jones

Pérez

et al. 2011

Monthly Notices of the Royal Astronomical Society

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“…The cold gas distribution is tightly correlated with the distribution of the SFR. Several groups have already measured the SFR in several regions along the disc of M33 using different tracers, including Hα emission and luminosity in the FUV and far‐infrared (FIR) bands (Engargiola et al ; Hippelein et al ; Heyer et al ; Boissier et al ; Gardan et al ; Verley et al ). The observed data of the radial distribution of SFR surface densities are plotted in the middle panel of Fig.…”

Section: The Observationsmentioning

confidence: 99%

The evolution and star-formation history of M33

Kang

Chang

Yin

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We construct a parametrized model to explore the main properties of the star-formation history of M33. We assume that the disc originates and grows by primordial gas infall and adopt a simple form of gas accretion rate with one free parameter, the infall time-scale. We also include the contribution of the gas outflow process. A major update of the model is that we adopt a molecular-hydrogen-correlated star-formation law and calculate the evolution of the atomic and molecular gas separately. Comparisons between the model predictions and observational data show that the model predictions are very sensitive to the adopted infall time-scale, while the gas-outflow process mainly influences the metallicity profile. A model adopting a moderate outflow rate and an inside-out formation scenario can be in good agreement with most of the observed constraints of the M33 disc. We also compare model predictions based on a molecular-hydrogen-correlated star-formation law and that based on the Kennicutt starformation law. Our results imply that the molecular-hydrogen-correlated star-formation law should be preferred to describe the evolution of the M33 disc, especially the radial distributions of both the cold gas and the stellar population.

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“…Boissier et al (2007) showed that most of the UV azimuthal profiles were extending quite smoothly beyond the optical radius, where it was thought previously that star formation was indeed present but only rare and stochastic (e.g., ). 2.2, various theories for star formation predict the existence of a threshold, or a critical surface density of gas Σ crit below which star formation should not proceed.…”

Section: Observed Thresholdsmentioning

confidence: 63%

Planets, Stars and Stellar Systems

Oswalt¹,

Keel²

2013

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Data Aggregation and Unification

Cited by 6 publications

References 4 publications

Age patterns in a sample of spiral galaxies

Age patterns in a sample of spiral galaxies

The evolution and star-formation history of M33

Planets, Stars and Stellar Systems

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