Detecting planets around very cool dwarfs at near infrared wavelengths with the radial velocity technique

F. Rodler; C. del Burgo; S. Witte; Ch. Helling; P. H. Hauschildt; E. L. Martín; C. Álvarez; R. Deshpande

doi:10.1051/0004-6361/201015490

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Volume 532 (August 2011)

A&A, 532 (2011) A31

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Table 1

Radial velocity precisions of the dwarfs that can be attained for spectral resolving powers R and SNR in the stellar continua.

R	SNR				RV precision (m s^-1)
	Y	J	H	K	Y	J	H	K

	M9.5V-dwarf (T_eff = 2200 K) + Case A
20 000	139	180	171	152	22.2	25.5	22.8	27.9
40 000	98	127	121	108	6.9	8.7	7.8	10.8
60 000	80	104	99	88	4.2	5.7	5.1	3.8
80 000	70	90	85	76	3.3	4.0	3.8	5.1

	M9.5V-dwarf (T_eff = 2200 K) + Case B
20 000	139	180	171	152	24.2	29.7	29.1	39.3
40 000	98	127	121	108	8.7	12.2	11.9	17.3
60 000	80	104	99	88	5.4	7.1	6.8	10.7
80 000	70	90	85	76	3.8	5.2	5.1	7.9

	L-dwarf (T_eff = 1800 K) + Case A
20 000	68	90	88	84	83.2	73.8	92.5	92.5
40 000	47	64	63	59	60.6	56.8	66.9	66.9
60 000	38	52	52	50	49.0	45.1	53.5	53.5
80 000	33	45	44	42	42.3	37.5	57.0	57.0

	L-dwarf (T_eff = 1800 K) + Case B
20 000	68	90	88	84	87.6	77.0	109.2	158.3
40 000	47	64	63	59	65.9	61.8	84.2	114.5
60 000	38	52	52	50	55.3	50.9	70.0	95.6
80 000	33	45	44	42	47.3	41.4	60.7	79.8

Notes. Case A shows the data analysis case of a complete and perfect removal telluric contamination, while Case B lists the RV precisions for the data analysis, where the telluric lines of a absorption depth of ≥ 3% were masked out.

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