Direct imaging of extra-solar planets in star forming regions - Lessons learned from a false positive around IM Lupi

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Table 2

Observing log for IM Lup and the reference stars used in this work.

Target	Prog. ID	α (J2000)	δ (J2000)	Filter	UT date	Exp. time	Tel./instr.	Strat.^a	Strehl (%)^b

IM Lup	10177	15^h56′09′′	–37°56′06′′	F160W	29/03/05	1350 s	HST/NICMOS	ADI	–
IM Lup	380.C-0910(A)	15^h56′09′′	–37°56′06′′	Ks	29/03/08	1350 s	VLT/NACO	RDI	58 ± 5
CD-37 8989	380.C-0910(A)	13^h54′27′′	–38°14′54′′	Ks	29/03/08	1200 s	VLT/NACO	–	50 ± 3
CD-35 9033	380.C-0910(A)	13^h50′00′′	–36°33′40′′	Ks	30/03/08	1200 s	VLT/NACO	–	48 ± 3
IM Lup	084.C-0444D	15^h56′09′′	–37°56′06′′	Lp	19/04/10	1350 s	VLT/NACO	RDI	80 ± 5
LHS3286	084.C-0444D	17^h23′49′′	–32°15′16′′	Lp	19/04/10	1350 s	VLT/NACO	–	85 ± 5
IM Lup	287.C-5040(A)	15^h56′09′′	–37°56′06′′	Ks	22/07/11	1350 s	VLT/NACO	I	40 ± 3
IM Lup	287.C-5040(A)	15^h56′09′′	–37°56′06′′	H	25/07/11	1350 s	VLT/NACO	I	30 ± 3

Notes. Note that all targets were observed at airmass ≃ 1.1, except for HST of course.

^(a)

Observing strategy: ADI (angular differential imaging), RDI (reference star differential imaging), I (imaging).

^(b)

The Strehl ratio was measured on the reduced image, or on the acquisition PSF (for saturated or coronagraphic data). Seeing and coherence time (τ₀) conditions in the Visible (≃0.5 μm) were very good for all observations, typically , and 3–8 ms, respectively.

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