Water in star-forming regions with Herschel (WISH) - VI. Constraints on UV and X-ray irradiation from a survey of hydrides in low- to high-mass young stellar objects

A. O. Benz; S. Bruderer; E. F. van Dishoeck; M. Melchior; S. F. Wampfler; F. van der Tak; J. R. Goicoechea; N. Indriolo; L. E. Kristensen; D. C. Lis; J. C. Mottram; E. A. Bergin; P. Caselli; F. Herpin; M. R. Hogerheijde; D. Johnstone; R. Liseau; B. Nisini; M. Tafalla; R. Visser; F. Wyrowski

doi:10.1051/0004-6361/201525835

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Volume 590 (June 2016)

A&A, 590 (2016) A105

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Table B.1

Observed line parameters of objects.

	T _max	rms	T _b	ΔV	V _line	δV		T _ex	N _i
	[K]	[K]	[K]	[km s^-1]	[km s^-1]	[km s^-1]	@ = ^∫τdV	[K]	[cm^-2]

CH⁺(1–0)
835.1375 GHz

NGC 1333 I2A	−0.088	0.015	0.14	4.9	5.6	−1.9	3.8^@	9	1.1(13)
NGC 1333 I4A	−0.071	0.016	0.21	5.6	5.8	−1.1	2.7^@	9	8.0(12)
NGC 1333 I4B	−0.032	0.014	0.11	6.0	6.0	−1.0	1.3^@	9	2.9(12)
Ser SMM1	−0.096	0.013	0.25	7.3	4.1	−4.1	5.8^@	9	1.7(13)
L 1489	>–0.030	0.010	0.014	−	−	−	<6.3^@	9	<1.9(13)
NGC 7129 FIRS2	−0.043	0.017	0.14	14.5	−5.4	4.5	2.4^@	9	7.0(12)

W3 IRS5	−1.3	0.009	0.89	7.1	−38.5	−0.1	10.0^@	8^a	4.4(13)^a
	2.1	0.009	0.89	3.0	−34.5	3.9	9.8	38^a	9.6(12)^a
NGC 6334 I	−3.6	0.030	3.7	5.9	−2.6	5.1	>48^@	7^a	2.6(14)^a DC
	−2.2	0.030	3.7	4.5	−11	−3.3	1.6^@	12^a	5.7(13)^a
NGC 6334 I(N)	−2.5	0.014	2.3	3.5	−1.9	2.6	<34^@	9	≤1.0(14)
	−1.5	0.014	2.3	7.1	6.5	11.0	4.9^@	9	1.5(13) DC
AFGL 2591	−0.28	0.010	0.47	10.3	−16.0	−10.5	8.7^@	3^a	1.8(14)^a
	0.33	0.010	0.47	13.5	−7.5	−2.0	0.86	43^a	8.5(12)^a
S 140	−0.30	0.030	−	2.7	−9.5	−2.4	2.1–20.1^@	9	0.6–5.9(13)
	0.27	0.030	−	1.9	−7.0	0.1	<0.38–2.4	38	0.16–1.0(12)
NGC 7538 IRS1	0.63	0.014	0.91	13.5	−57.5	−0.1	9.3	44^a	4.1(12)^a
	−0.90	0.014	0.91	8.8	−51.8	5.6	8.7^@	3^a	1.1(14)^a

CH⁺(2–1)
1669.2813 GHz

NGC 1333 I2A	<0.17	0.058		−	−	−	<0.48
NGC 1333 I4A	<0.17	0.058		−	−	−	<0.49
NGC 1333 I4B	<0.18	0.061		−	−	−	<0.51
Ser SMM1	<0.22	0.074		−	−	−	<0.63

W3 IRS5	1.1	0.045	4.1	7.7	−35.9	2.5	8.7
NGC 6334 I	−2.8	0.12	11.4	3.9	−10.3	−2.6	1.15^@
	−0.92	0.16	11.4	4.5	−2.5	5.2	0.36^@
NGC 6334 I(N)	<0.31	0.11	1.7	−	−	−	<0.87
AFGL 2591	0.85	0.077	2.3	8	−4.6	0.9	3.7
NGC 7538 IRS1	0.41	0.12	2.9	10.7	−57.7	0.3	2.7

OH⁺ (1–0)
1033.1186 GHz

NGC 1333 I2A	<0.055	0.018	0.26	−	−	−	<-0.59^@	9	<5.2(12)
NGC 1333 I4A	−0.040	0.020	0.25	1.4	4.1	−2.8	≤0.2^@	9	≤1.9(12)
NGC 1333 I4B	−0.043	0.019	0.17	1.7	1.8	−5.2	≤0.63^@	9	≤5.7(12)
Ser SMM1	−0.20	0.065	0.43	9.7	4.8	−3.7	8.3^@	9	7.3(13)
L 1489	<0.50	0.017	0.037	−	−	−	<3.9^@	9	<3.4(13)
NGC 7129 FIRS2	−0.024	0.021	0.22	7.4	−1.9	8.0	1.0^@	9	8.8(12)

W3 IRS5	−0.2	0.015	1.7	5.9	−42	−3.6	0.99^@	9	8.8(12)
	0.1	0.015	1.7	9.4	−33	5.4	0.50	38	5.9(11)
NGC 6334 I	−0.55	0.031	6.0	5.9	−10.0	−2.3	0.66^@	9	5.2(12)
	−2.1	0.031	6.0	6.4	−1.6	6.1	2.8^@	9	2.3(13) DC
NGC 6334 I(N)	−0.99	0.021	3.0	4.9	−1.6	2.9	3.8^@	9	3.3(13)
	−1.35	0.021	3.0	3.5	3.2	7.7	3.7^@	9	3.3(13) DC
AFGL 2591	−0.14	0.016	0.90	11.8	−16.1	−10.6	1.0^@	3^a	1.6(13)^a
	−0.71	0.016	0.90	9.4	2.8	8.3	3.6^@	3^a	6.1(13)^a DC
S 140	−0.30	0.024	0.96	4.5	−4.1	3.0	1.5^@	9	1.8(13)
	−0.18	0.024	0.96	6.7	3.5	10.6	1.3^@	9	1.5(13) DC
NGC 7538 IRS1	−0.18	0.026	1.6	12.0	−48	9.4	1.6^@	9	1.4(13)

Notes. T_max refers to the line peak intensity, negative values indicate absorption in [K] below background; ΔV to the FWHM line width; V_line to the line mean velocity; δV = V_line − V_LSR to the line shift with respect to the systemic velocity of the object; rms to the root mean square noise level; T_b to the background (continuum) intensity; the integrated line flux (line luminosity) is given in [K km s^-1]), @ indicates integrated optical depth [km s^-1]; T_ex is the assumed excitation temperature; and N_i is the total column density. Cases where the fitted line model had to be used for intensity or absorption instead of the observed data because of line blending are indicated with an asterisk (*), and values labeled (a) are from 1D slab model fitting (Bruderer et al. 2010a,Appendix B). A minus sign (−) indicates observations but no detection. Absorption components indicated with “DC” are suspected to originate from diffuse interstellar clouds in the foreground. The error range in emission measure is up to factors of 0.8–2 for emission lines, and factors of 0.8–1.5 for lines in absorption. Details and error margins of the column densities are given in Sect. 4 and Table 3.

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