Redshifted X-rays from the material accreting onto TW Hydrae: Evidence of a low-latitude accretion spot

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Table 3

Emission lines selected for Doppler shift measurements.

Index^a	λ ^b	Elem.	T _max	Flux contrib.^c		Line

	(Å)		(MK)	Accr.	Cor.	subset^d

1a	6.1804	Si xiv	15.8	0.00	1.00	h
1b	6.1858	Si xiv	15.8	0.00	1.00	h
2	6.6479	Si xiii	10.0	0.01	0.99	h
3	6.7403	Si xiii	10.0	0.02	0.98	h
4a	8.4192	Mg xii	10.0	0.00	1.00	h
4b	8.4246	Mg xii	10.0	0.00	1.00	h
5	9.1687	Mg xi	6.3	0.31	0.69	h
6a	9.7080	Ne x	6.3	0.07	0.93	h
6b	9.7085	Ne x	6.3	0.07	0.93	h
7a	10.2385	Ne x	6.3	0.09	0.91	h
7b	10.2396	Ne x	6.3	0.09	0.91	h
8	13.6990	Ne ix	4.0	0.96	0.04	c
9	15.0140	Fe xvii	5.0	0.73	0.27	h
10a	16.0055	O viii	3.2	0.92	0.08	c
10b	16.0067	O viii	3.2	0.92	0.08	c
11	16.7800	Fe xvii	5.0	0.77	0.23	h
12	17.0510	Fe xvii	5.0	0.76	0.24	h
13	17.0960	Fe xvii	5.0	0.78	0.22	h
14a	18.9671	O viii	3.2	0.94	0.06	c
14b	18.9725	O viii	3.2	0.94	0.06	c
15	21.6015	O vii	2.0	1.00	0.00	c

Notes.

^(a)

Lines indicated with the same index number, but different letters, are the two components of H-like resonance doublets.

^(b)

APED predicted wavelengths.

^(c)

Fractional contributions to individual line fluxes due to accretion and corona components, on the basis of the model C obtained by Brickhouse et al. (2010).

^(d)

“c” and “h” indicate whether the line has been included in the cool or hot line subsample.

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