2009A&A...495..479C


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.05CEST06:25:43

2009A&A...495..479C - Astronomy and Astrophysics, volume 495, 479-490 (2009/2-4)

The cluster birthline in M33.

CORBELLI E., VERLEY S., ELMEGREEN B.G. and GIOVANARDI C.

Abstract (from CDS):

The aim of this paper is twofold: (a) to determine the reliability of infrared (IR) emission to trace star formation in individual star-forming sites of M33, and (b) to outline a new method for testing the distribution function of massive stars in newly formed clusters. We select 24µm IR sources from the Spitzer survey of M33 with Hα counterparts and show that the IR luminosities have a weak dependence on galactocentric radius. The IR and Hα luminosities are not correlated. Complementing the infrared photometry with GALEX-UV data, we estimate the bolometric luminosities to investigate how they are related to the Hα luminosities. We simulate a theoretical diagram for the expected bolometric-to-Hα luminosity ratio, Lbol/L, of young clusters as a function of the cluster luminosity. We then compare the observed Lbol/L ratios with the theoretical predictions. In the log(Lbol)-log(Lbol/L) plane, stellar clusters should be born along a curve that we call the cluster birthline. The birthline depends on the stellar initial mass function (IMF) at the high-mass end, but not on the cluster mass function. For an upper stellar mass limit of 120M, the birthline is flat for Lbol>3x1039erg/s because all clusters fully sample the IMF. It increases toward lower luminosities as the upper end of the IMF becomes incompletely sampled. Aging moves clusters above the birthline. The observations of M33 show that young isolated clusters lie close to the theoretical birthline for a wide range of Lbol. The observed Lbol/L ratio increases toward low Lbol like the theoretical curve, indicating that luminosity is not proportional to Hα emission for low mass clusters. The best fit to the birthline is for a randomly sampled IMF, in which the mass of most massive star in a cluster is not strictly limited by the cluster's mass, but can have any value up to the maximum stellar mass with a probability determined by the IMF. We also find that the IR luminosity of young stellar clusters in M33 is not proportional to their bolometric luminosity. This irregularity could be the result of low and patchy dust abundance. In M33 dust absorbs and re-radiates in the IR only part of the UV light from young clusters.

Abstract Copyright:

Journal keyword(s): stars: luminosity function, mass function - dust, extinction - galaxies: star clusters - galaxies: individual: M33

Simbad objects: 7

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Number of rows : 7

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 10902 1
2 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9440 1
3 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5134 1
4 NGC 604 HII 01 34 32.1 +30 47 01           ~ 544 0
5 M 51 GiP 13 29 52.698 +47 11 42.93   9.26 8.36 8.40   ~ 3781 4
6 NGC 6822 G 19 44 56.199 -14 47 51.29   18 8.1     ~ 1428 0
7 NAME Local Group GrG ~ ~           ~ 6970 0

    Equat.    Gal    SGal    Ecl

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2020.07.05-06:25:43

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