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Cited by 26 publications
(35 citation statements)
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“…The standard deviation in the measured distribution is 0.91, and the authors estimate the standard error of their method to be 0.51. Therefore the measured distribution of slopes is meaningful [34]. Because the total number of analysed star formation complexes is rather large, the formal probability of measuring such a large standard deviation is basically negligible (< 10 −10 ), if one assumes a universal IMF.…”
Section: Extragalactic Star Formation Complexesmentioning
confidence: 99%
See 1 more Smart Citation
“…The standard deviation in the measured distribution is 0.91, and the authors estimate the standard error of their method to be 0.51. Therefore the measured distribution of slopes is meaningful [34]. Because the total number of analysed star formation complexes is rather large, the formal probability of measuring such a large standard deviation is basically negligible (< 10 −10 ), if one assumes a universal IMF.…”
Section: Extragalactic Star Formation Complexesmentioning
confidence: 99%
“…A recent example for such a statistical approach is [34], who have included 105 extragalactic star formation complexes for which UBVR photometry, Lyman continuum flux, metallicity and extinction measurements were available. These properties trace essentially the high mass stellar content, and the results are restricted to the IMF for stars more massive than 10 M ⊙ .…”
Section: Extragalactic Star Formation Complexesmentioning
confidence: 99%
“…Figure 1 shows the H I map overlaid with the footprints of 29 Hubble Space Telescope (HST) fields. We also use the Hα (KPNO; Hoopes et al 2001) and 24 μm (Spitzer; Dale Rots (1975) 12 Roberts et al (1975) 11.5 Visser (1980) 13 Sakhibov & Smirnov (1987) >12.86 Elmegreen et al (1989) 9.84 Lowe et al (1994) 10.52 Westpfahl (1998) 9.8 Kendall et al (2008) 12.67 Tamburro et al (2008) 9. 23 Feng et al (2014) 9.5…”
Section: Datamentioning
confidence: 99%
“…In turn, NGC 253 is a starburst galaxy with a rather high disk inclination, inappropriate for tracing spiral arms. However, later works by Sakhibov & Smirnov (1987, 1989, 1990 made it evident that the main problem of these early approaches is that independent determination of the rotation curve and of the residual velocities related to a density wave is not possible even for an "ideal" two-armed grand design galaxy. This conclusion was based on the analysis of the line-of-sight velocity fields of some galaxies by applying a Fourier-series expansion of velocity along the galactocentric azimuthal angle.…”
Section: Introductionmentioning
confidence: 99%