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Verfasst von:Haydon, Daniel T. [VerfasserIn]   i
 Kruijssen, Diederik [VerfasserIn]   i
 Chevance, Mélanie [VerfasserIn]   i
 Hygate, Alexander P. S. [VerfasserIn]   i
 Krumholz, Mark R. [VerfasserIn]   i
 Schruba, Andreas [VerfasserIn]   i
 Longmore, Steven N. [VerfasserIn]   i
Titel:An uncertainty principle for star formation
Titelzusatz:III. The characteristic emission time-scales of star formation rate tracers
Verf.angabe:Daniel T. Haydon, J.M. Diederik Kruijssen, Mélanie Chevance, Alexander P.S. Hygate, Mark R. Krumholz, Andreas Schruba and Steven N. Longmore
E-Jahr:2020
Jahr:17 August 2020
Umfang:23 S.
Fussnoten:Gesehen am 13.01.2021
Titel Quelle:Enthalten in: Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society
Ort Quelle:Oxford : Oxford Univ. Press, 1827
Jahr Quelle:2020
Band/Heft Quelle:498(2020), 1, Seite 235-257
ISSN Quelle:1365-2966
Abstract:We recently presented a new statistical method to constrain the physics of star formation and feedback on the cloud scale by reconstructing the underlying evolutionary timeline. However, by itself this new method only recovers the relative durations of different evolutionary phases. To enable observational applications, it therefore requires knowledge of an absolute ‘reference time-scale’ to convert relative time-scales into absolute values. The logical choice for this reference time-scale is the duration over which the star formation rate (SFR) tracer is visible because it can be characterized using stellar population synthesis (SPS) models. In this paper, we calibrate this reference time-scale using synthetic emission maps of several SFR tracers, generated by combining the output from a hydrodynamical disc galaxy simulation with the SPS model slug2. We apply our statistical method to obtain self-consistent measurements of each tracer’s reference time-scale. These include H α and 12 ultraviolet (UV) filters (from GALEX, Swift, and HST), which cover a wavelength range 150-350 nm. At solar metallicity, the measured reference time-scales of H α are ${4.32^{+0.09}_{-0.23}}$ Myr with continuum subtraction, and 6-16 Myr without, where the time-scale increases with filter width. For the UV filters we find 17-33 Myr, nearly monotonically increasing with wavelength. The characteristic time-scale decreases towards higher metallicities, as well as to lower star formation rate surface densities, owing to stellar initial mass function sampling effects. We provide fitting functions for the reference time-scale as a function of metallicity, filter width, or wavelength, to enable observational applications of our statistical method across a wide variety of galaxies.
DOI:doi:10.1093/mnras/staa2430
URL:Bitte beachten Sie: Dies ist ein Bibliographieeintrag. Ein Volltextzugriff für Mitglieder der Universität besteht hier nur, falls für die entsprechende Zeitschrift/den entsprechenden Sammelband ein Abonnement besteht oder es sich um einen OpenAccess-Titel handelt.

Volltext: https://doi.org/10.1093/mnras/staa2430
 DOI: https://doi.org/10.1093/mnras/staa2430
Datenträger:Online-Ressource
Sprache:eng
K10plus-PPN:174453490X
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