The nature of the Class I population in Ophiuchus as revealed through gas and dust mapping

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Volume 498 / No 1 (April IV 2009)

A&A, 498 1 (2009) 167-194

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Table 4:

Source fluxes including IRAC 1-4, MIPS 1-2, SHARC-II, SCUBA and 1.3 mm data.
Source	3.6 $\mu$ m^e	4.5 $\mu$ m^e	5.8 $\mu$ m^e	8.0 $\mu$ m^e	24 $\mu$ m^e	70 $\mu$ m	350 $\mu$ m	450 $\mu$ m	850 $\mu$ m	850 $\mu$ m	1300 $\mu$ m
	IRAC I	IRAC II	IRACIII	IRAC IV	MIPS I	MIPS II	SHARC	SCUBA	SCUBA	SCUBA
						$\sim$ 10''	9-25''^b	10 ''^b	15''	25''	15''
	mJy	mJy	mJy	mJy	mJy	mJy	mJy	mJy	mJy	mJy	mJy
C2D-162527.6	1.15e1	1.77e1	3.00e1	6.03e1	8.51e1	-	-	-	<3e1	<3e1
GSS 26	2.86e2K	3.86e2K	5.09e2	6.17e2	7.98e2	-		6.5e2	3.0e2^b	1.6e3	1.e2
CRBR 2315.8-1700	4.53e1	8.77e1	1.61e2	2.37e2	5.16e2	-	-		2.1e2	7.5e2	8.5e1)
CRBR 2317.3-1925	1.05e1	1.15e1	1.39e1	2.05e1	1.46e1	-			1.5e2^b	1.7e2
VSSG 1	7.57e2	1.01e3	9.67e2	9.96e2	9.48e2	-		<6.7e2	2.4e2^b	3.0e2	5e1
GSS 30	1.06e3	2.27e3	4.1e3	5.4e3	-	7.83e4	2.5e3^a	1.4e3	2.2e2^b	3.2e2	9e1
LFAM 1	1.28e1	1.82e1*	3.78e1	1.59e1*	2.41e2*	6.31e4		2.7e3	5.7e2^b	2.6e3	1.1e3
CRBR 2324.1-1619	9.37e0	1.59e1	2.17e1	2.95e1	4.47e2	-			8.4e2	6.1e3
VLA 1623	-	1.57e-1*	2.45e-1*	-	4.04e1	-	4e5^c	3.9e5^c	5.0e3	1.7e4	1.2e3
GY51	2.86e2	3.71e2	4.38e2	4.66e2	6.39e2*	-			3.3e2	1.7e3	2e1
CRBR 2339.1-2032	3.04e1	4.48e1	6.05e1	8.28e1	3.93e2	-			8e1	3e2	3e2
WL 12	2.39e2	7.44e2	1.61e3	2.24e3	-	7.0e3	6.7e3^a	7.5e2	2.2e2^b	7.1e2	1.2e2
WL 2	7.92e1	1.11e2	1.28e2	1.48e2	4.46e2	-			4e1	1.4e2	3e1
LFAM 26	6.11e0	1.07e1	1.66e1	2.96e1	4.59e2	-			2.2e2	6.9e2	1e2
WL 17	2.4e2	4.16e2	5.53e2	6.95e2	2.79e3	6.8e3		<8.7e2	1e2^b	6.1e2	7.5e1
Elias 29	-	-	1.28e4	-	-	<4.7e4	4.3e3^a	2.0e3	4.1e2^b	9.4e2	9.5e1
GY 224	2.03e2	3.05e2K	3.58e2	3.67e2	9.07e2				1.3e2	3.7e2	5e1
WL19	2.15e2	3.54e2K	4.06e2	3.28e2	2.23e2	-			2.0e2	8.3e2	3e1
WL 20S	6.53e-1*^d	2.97e1	3.74e1*	2.43e2	1.46e2*	1.4e4	8.2e2^a	4.0e2	1.8e2^b	6.0e2	4.7e1
IRS 37	1.27e2	2.06e2	2.86e2	2.68e2	7.8e2	1.4e4		<5.9e2	9.3e1^b	3.0e2	<1e1
WL 3	9.86e1	1.63e2	2.08e2	2.04e2	3.25e2	<2.4e4		<5.8e2	1.2e2^b	4.4e2	<6e1
IRS 42	1.06e3	1.63e3	2.1e3	2.98e3	3.45e3	3.0e3	1.5e3^a		1.7e2	7.3e2	<6e1
WL 6	4.67e2K	9.25e2	1.44e3	1.73e3	4.36e3	3.5e3		1.4e2	<3e1	<3e1	<2e1
GY 256	1.09e1	1.19e1	1.38e0*	8.58e-1*	2.86e1*	3.5e3			<3e1	<3e1
IRS 43	6.29e2	1.24e3	1.79e3	2.19e3	-	2.4e4	2.1e3^b	1.8e3	2.5e2^b	2.7e3	8e1
IRS 44	7.31e2	1.83e3	2.94e3	2.32e3	-	2.5e4			3.6e2	1.2e3	6e1
Elias 32	1.87e2	2.72e2	3.82e2	4.81e2	7.12e2	1.1e4			1.7e3	6.4e3	<5e1
Elias 33	7.4e2	1.19e3	1.58e3	2.04e3	1.72e3	<1.0e4	4.4e3^a		1.2e3	4.4e3	<2e1
IRS 48	1.41e3	1.6e3	4.06e3	6.0e3	-	1.7e4		<1.6e3	1.8e2^b	1.9e2	6e1
GY 312	1.58e1	2.67e1	3.82e1	5.32e1	4.61e2	7.1e2			<3e1	<3e1
IRS 51	7.52e2	9.16e2	1.00e3	1.07e3	2.73e3	2.4e3	1.4e3^a	<6.8e2	2.2e2	7.8e2	1.1e2
C2D-162741.6	8.31e0	1.39e1	2.04e1	2.86e1	6.89e1	5.3e2			1e2	3.5e2
C2D-162748.2	1.21e0	2.21e0	3.64e0	1.41e1	1.84e2				5e1	6e1
IRS 54	5.25e2K	7.12e2	9.31e2	1.01e3	3.56e3	5.0e3			1e2	3.2e2	3e1
IRAS 16285	5.89e-1	2.55e0	4.49e0K	3.13e0	9.01e1	1.7e3			5e2	1.6e3
C2D-162857.9	9.73e0	1.7e1	2.57e1	3.83e1	1.61e2	-			5e1	8.5e2
IRS 63	5.89e2	9.57e2	1.25e3	1.45e3	3.23e3	8.3e3	6.7e3^b	4.7e3	1.0e3^b	2.4e3	3.7e2
Disks
Haro 1-4	5.19e2	-	3.73e2	-	8.39e2	5.6e2			-	-
DoAR 25	3.67e2	2.92e2	2.99e2	2.58e2	3.99e2	1.4e3			4.6e2^b	5.2e2	2.8e2
OphE MM3	1.42e0	1.79e0	1.88e0*	2.22e0	1.41e0*	-	1.6e3^a	5.4e2	1.6e2	3.6e2
SR 21	1.3e3	1.17e3	1.28e3	1.66e3	-	1.3e3	2.8e3^b	1.9e3	4.0e2^b	4.7e2	9.5e1
CRBR 2422.8-3423	5.4e1	1.31e2	1.91e2	1.98e2	1.34e3	9.8e3			1.3e3	3.2e3	1.5e2
IRS 46	1.72e2K	2.71e2	4.02e2	4.11e2	6.39e2*	-	1.4e3^a		1.8e2	5.1e2	4.5e1
SR 9	7.84e2	5.75e2	4.65e2	4.84e2	1.04e3	-			<25^b	2.9e1	1.5e1
2Mass 16282	2.32e0	2.00e0	1.39e0	8.15e-1	1.58e0	-	9e1^b	8e1	5.8e1	2.7e2

^a This paper; ^b 350/450 $\mu$ m flux taken from Andrews & Williams (2007). Fluxes obtained with SHARC-II are given either in a 9'' beam (Andrews & Williams 2007) or in a 25'' radius (This work); ^c data taken from André et al. (1993); ^d two sources within 4'' with a total flux of 2e2 mJy; ^e IRAC and MIPS-24 Fluxes marked with ``*'' are band-filled sources with a S/N < 5 or sources with S/N < 5. Such limits are caused either by saturation or a very low emission. A ``K'' added to the flux indicates that the obtained flux was flagged as ``Complex'', with multiple detection within 2-3''.

Source LaTeX | All tables | In the text

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