No evidence for significant age spreads in young massive LMC clusters

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Volume 575 (March 2015)

A&A, 575 (2015) A62

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Table 1

Parameters of the LMC clusters.

Cluster	Age (Myr)		log Mass/ M_⊙	Z (Z_⊙ = 0.0152)		R_core (pc)	V_esc (km s^-1)	V_esc (km s^-1)	E(B − V)
	lit.	this work		lit.	this work			at 10 Myr	lit.	this work


NGC 1831	700^a	926	4.59^b	0.016^a	0.016	4.24^c/4.13^b	6.6^b	9.3	0.01^a	0.0
NGC 1847	26^d	57	4.44^b	0.006^e	0.006	3.35^c/1.73^b	4.2^b	4.5	0.1^f	0.16
NGC 1850	30^g	93	4.86^b/5.15	0.008^h	0.006	−−/2.69^b	8.77^b/12.3	15.5	0.17^h	0.1
NGC 2004	20ⁱ	20	4.36^b	0.004^j	0.004	2.18^c/1.41^b	7.0^b	7.5	0.08^k	0.23
NGC 2100	16ⁱ	21	4.36^b	0.007^j	0.007	3.03^c/0.99^b	7.9^b	8.5	0.24^k	0.17
NGC 2136	100^l	124	4.30^b	0.004^l	0.005	2.91^c/1.59^b	7.4^b	9.3	0.1^l	0.13
NGC 2157	100^m	99	4.31^b	0.008^m	0.008	−−/2.00^b	6.2^b	7.8	0.1^m	0.1
NGC 2249	1000ⁿ	1110	4.48ⁿ	0.007^a	0.008	2.79^c/1.75^b	9.4ⁿ	12.1	0.01^a	0.02


NGC 1856	281^o		4.88^b	0.008^o		−−/1.75^b	11.0^b	14.7	0.26^o
NGC 1866	177^o		4.91^b	0.008^o		−−/2.79^b	9.5^b	12.5	0.05^o

Notes. In the columns that give the age, the metallicity Z and the extinction E(B − V), the first value is from the literature and the second one is determined in this work. Additionally, we also found new values for the mass and the escape velocity of NGC 1850 (second values in the respective columns). The core radius of the clusters can be determined in two ways: using the surface number density (first value) or the surface brightness density (second value). The last two clusters (NGC 1856 and NGC 1866) are not studied in this work. They were already analyzed by Bastian & Silva-Villa (2013).

Reference.

^(a)

Kerber et al. (2007);

^(b)

McLaughlin & van der Marel (2005) assuming King (1966) profiles;

^(c)

Brocato et al. (2001);

^(d)

Elson & Fall (1988);

^(e)

Mackey & Gilmore (2003);

^(f)

Nelson & Hodge (1983);

^(g)

Baumgardt et al. (2013);

^(h)

Fischer et al. (1993);

⁽ⁱ⁾

Elson (1991);

^(j)

Jasniewicz & Thevenin (1994);

^(k)

Keller et al. (2000);

^(l)

Dirsch et al. (2000);

^(m)

Fischer et al. (1998);

⁽ⁿ⁾

Correnti et al. (2014);

^(o)

Bastian & Silva-Villa (2013).

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