Tracing the sites of obscured star formation in the Antennae galaxies with Herschel-PACS

Free Access

Table 1:

Integral fluxes and fluxes of the emission knots from the ISOCAM 15 $\mu$ m, *Spitzer*-MIPS 24 $\mu$ m, and *Herschel*-PACS 70, 100, and 160 $\mu$ m maps.
knot ID	fluxes (mJy)
	15 $\mu$ m	24 $\mu$ m	70 $\mu$ m	100 $\mu$ m	160 $\mu$ m
integral	1720	5960	67 200	102 000	95 500
NS	34.8	72.0	1726	1728	1489
K1	341.5	1282	8144	8567	5030
K2a	61.0	159.9	2529	4004	6894²
K2b+c	81.2	251.9	3474	5999
K3a	14.0	43.0	529.1	1549¹	-
K3b	7.8	21.9	316.1		-
K4	20.2	39.9	742.6	847.5	509.1
NN	84.7	260.7	3360	4904	4470
A1a+b	17.5	34.0	708.2	858.4	500.7
A2	6.0	17.9	282.4	508.0	-
A3	48.0	116.4	1695	1699	1353
A4b	12.1	20.5	698.6	693.8	744.6³
A4c	5.3	19.9	216.3	368.8
A4d	3.8	5.9	81.6	-	-
A5a	3.3	5.7	64.9	340.2¹	441.1²
A5b	3.7	4.5	66.5
A5c	2.7	4.9	110.5	237.9
A6	9.2	26.8	269.9	318.6	-

Notes. The labelling of the knots follows Fig. 3. The photometric accuracy is estimated to be $\pm$ 20%. ⁽¹⁾ a+b; ⁽²⁾ a+b+; ^(c) b+c.

Source LaTeX | All tables | In the text

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.