scholarly journals The galaxy-wide initial mass function of dwarf late-type to massive early-type galaxies

2013 ◽  
Vol 436 (4) ◽  
pp. 3309-3320 ◽  
Author(s):  
C. Weidner ◽  
P. Kroupa ◽  
J. Pflamm-Altenburg ◽  
A. Vazdekis
2019 ◽  
Vol 490 (1) ◽  
pp. 848-867 ◽  
Author(s):  
J Dabringhausen

ABSTRACT The galaxy-wide stellar initial mass function (IGIMF) of a galaxy is thought to depend on its star formation rate (SFR). Using a catalogue of observational properties of early-type galaxies (ETGs) and a relation that correlates the formation time-scales of ETGs with their stellar masses, the dependencies of the IGIMF on the SFR are translated into dependencies on more intuitive parameters like present-day luminosities in different passbands. It is found that up to a luminosity of approximately 109 L⊙ (quite independent of the considered passband), the total masses of the stellar populations of ETGs are slightly lower than expected from the canonical stellar initial mass function (IMF). However, the actual mass of the stellar populations of the most luminous ETGs may be up to two times higher than expected from a simple stellar population model with the canonical IMF. The variation of the IGIMF with the mass of ETGs is presented here also as convenient functions of the luminosity in various passbands.


Author(s):  
Aaron A. Dutton ◽  
Charlie Conroy ◽  
Frank C. van den Bosch ◽  
Luc Simard ◽  
J. Trevor Mendel ◽  
...  

2014 ◽  
Vol 447 (2) ◽  
pp. 1033-1048 ◽  
Author(s):  
Ignacio Martín-Navarro ◽  
Francesco La Barbera ◽  
Alexandre Vazdekis ◽  
Jesús Falcón-Barroso ◽  
Ignacio Ferreras

2015 ◽  
Vol 12 (S316) ◽  
pp. 357-358
Author(s):  
Beomdu Lim ◽  
Hwankyung Sung ◽  
Hyeonoh Hur ◽  
Byeong-Gon Park

AbstractThe initial mass function (IMF) is an essential tool with which to study star formation processes. We have initiated the photometric survey of young open clusters in the Galaxy, from which the stellar IMFs are obtained in a homogeneous way. A total of 16 famous young open clusters have preferentially been studied up to now. These clusters have a wide range of surface densities (log σ = −1 to 3 [stars pc−2] for stars with mass larger than 5M⊙) and cluster masses (Mcl = 165 to 50, 000M⊙), and also are distributed in five different spiral arms in the Galaxy. It is possible to test the dependence of star formation processes on the global properties of individual clusters or environmental conditions. We present a preliminary result on the variation of the IMF in this paper.


2013 ◽  
Vol 764 (2) ◽  
pp. 155 ◽  
Author(s):  
J. R. Lu ◽  
T. Do ◽  
A. M. Ghez ◽  
M. R. Morris ◽  
S. Yelda ◽  
...  

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