Star formation in grand-design, spiral galaxies - Young, massive clusters in the near-infrared

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Volume 542 (June 2012)

A&A, 542 (2012) A39

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Table 1

List of galaxies.

Galaxy	Type	Bands	FWHM	μ₅	m − M	D	Δs	PA	IA	K_l	H_l	J_l	Y_l	N_s

NGC 157	Sc(s) I-II	YJHK	0.37	23.9	31.28	18.0	32	40^a	45^a	20.19	20.71	21.27	21.75	2254
NGC 1232	Sc(rs) I	YJHK	0.38	24.1	31.48	19.8	36	90^b	30^b	20.62	20.80	21.72	22.21	3177
NGC 1300	SBb(s) I.2	YJHK	0.55	24.0	31.46	19.6	52	87^c	35^c	19.80	20.30	21.18	21.30	614
NGC 1365	SBb(s) I	YJHK	0.40	23.7	31.62	21.1	41	40^d	40^d	20.17	20.32	21.24	21.73	2417
NGC 1566	Sc(s) I	YJHK	0.44	23.1	31.55	20.5	44	41^e	27^e	19.29	19.82	20.64	21.18	969
NGC 2997	Sc(s) I.3	YJHKBr_γ	0.38	23.8	31.42	19.2	35	107^f	32^f	20.14	20.33	21.27	21.75	5313
NGC 4030	Sbc(r) I	YJHK	0.44	23.6	31.99	25.0	53	27^g	44^g	19.70	20.19	20.76	21.26	1196
NGC 4321	Sc(s) I	YJHK	0.66	23.7	32.07	26.0	83	153^h	27^h	19.32	19.81	20.74	21.66	1184
NGC 5247	Sc(s) I-II	YJHK	0.41	23.7	31.77	22.6	45	97^h	29^h	19.79	20.65	21.26	21.75	2259
NGC 7424	Sc(s) II.3	JHK	0.41	24.3	29.88	9.5	19	44ⁱ	27ⁱ	20.80	21.23	22.21	–	6137

Notes. Name and Hubble type are listed as given in RSA. Filter bands observed, seeing in the final, stacked K-band image expressed as the full-width at half-maximum (FWHM) in arcsec, and K_s surface brightness μ₅ in magnitudes per pixel for which a signal-to-noise ratio of five was reached are also shown. The adopted distance modulus, m − M, distance D in Mpc, and the corresponding linear resolution Δs in pc are provided. The position angle PA and inclination angle IA adopted for the galaxies are listed in degrees. Limiting magnitudes K_l, H_l, J_l, and Y_l are indicated corresponding to a completeness of around 90% (see text). Finally, the total number of sources N_s in the galaxy disks for which aperture magnitudes could be estimated is given.

References. References to the projection parameters adopted: and

^(a)

Zurita et al. (2002);

^(b)

van Zee & Bryant (1999);

^(c)

Lindblad et al. (1997);

^(d)

Pence et al. (1990);

^(e)

Hess et al. (2009);

^(f)

Ganda et al. (2006);

^(g)

Knapen et al. (1993);

^(h)

Kuno et al. (2007);

⁽ⁱ⁾

Becker et al. (1988).

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