From large scale gas compression to cluster formation in the Antennae overlap region

C. N. Herrera; F. Boulanger; N. P. H. Nesvadba

doi:10.1051/0004-6361/201117324

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Volume 534 (October 2011)

A&A, 534 (2011) A138

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Table 1

Parameters of the super star cluster in our field.

Obs	Size	Age	A_K	Mass	N_ion	K	Reference
	″	Myr	mag	× 10⁶M_⊙	× 10⁵² s^-1	mag

HST	−	4.8^a	0.8^a^b	1.2^a	−	−	#28 from Table 8 in [1]
Keck + VLT	046^c	5.7^d	−	4.1^e	1.3^e	15.2^f	SSC-C in [2]
VLT/SINFONI	06^g	<6	0.4	6.0	4.4^e^h	15.0^f	Our work [3]
VLT/SINFONI	06^g	4.5	0.4	6.0	6.6ⁱ	15.0^f	Our work [3]

Notes.

^(a)

From the comparison of integrated photometry UBVIHα with population synthesis models,

^(b)

estimated from measured E(B − V) = 2.20 and assuming R_V = 3.1 extinction curve (Weingartner & Draine 2001),

^(c)

deconvolved FWHM from Lorentzian fit,

^(d)

based on the Brγ equivalent width as an age indicator comparing it with Starburst99 (Leitherer et al. 2010) models,

^(e)

not corrected for extinction,

^(f)

K-band apparent magnitude for an aperture of 2″,

^(g)

it is unresolved. The angular size (FWHM) measured from a Gaussian fit corresponds to the size of the seeing disk,

^(h)

from observed Brγ luminosity,

⁽ⁱ⁾

from the fluxes of the [Ne ii] and [Ne iii] lines at 12.81 and 15.56 μm.

References. [1] Whitmore et al. (2010) based on ACS and NICMOS observations, [2] Gilbert & Graham (2007) based on Keck/NIRSPEC-SCAM and VLT/ISAAC observations, [3] for details see Sect. 3.1.

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