SU Aur

SU Aur

Updated: February 21, 2012

Contribution: Joan Guarro, François Teyssier, Christian Buil

Call for observations from Hans Moritz Guenther (Harvard-Smithsonian Center for Astrophysics):

In a few days, I have an observation of SU Aur with XMM-Newton. SU Aur is relatively bright (m_V = 9.5). It's an accreting, young classical T Tauri star and we want to study the relation between X-ray flares and accretion.

Thus, I am looking for someone who can take Halpha spectroscopy (which traces the accretion) in short cadence during the XMM-Newton observation (in UT 2012-02-15@20:31:13 to 2012-02-17@01:27:53).

The Halpha line of SU Aur is very broad (~500 km/s) and bright (about 2 times the continuum level). See http://sprg.ssl.berkeley.edu/~cmj/html/suaur.html for examples of SU Aur's H alpha line in past observations.

Thus, a resolving power ~50-100 km/s = 3000-6000 is totally sufficient, but of course I don't say "no" to better spectrum. It would be very useful to obtain simultaneous spectroscopy of the Halpha line. However, short exposure times are also important, so that I can see if the Halpha line profile changes, when an X-ray flare happens.

Send your observations to: christian.buil_at_wanadoo.fr. Give a description of your instrument, evaluation of spectral resolution, exposure time and time of observation in UT.

Coordinates (2000.0) = RA : 04h 55m 59.38s - Dec : +30° 34' 01.52"

Log of observations

#	Date (DD/MM/YYY)	Observer	Telescope	Spectrograph	Camera	Exposure	Resolution	Range (A)	fits files
1	11.768 / 02 / 2012	F. Teyssier	D = 0.25 m	LISA	SXV-H9	4460 s	800	4000 - 7100	_suaur_20120211_768_teyssier.fit
2	11.808 / 02 / 2012	C. Buil	D= 0.28 m (C11)	LHIRES III 600 l/mm	Atik314L+	9 x 600 s	3400	6160 - 6860	_suaur_20120211_808_buil.fit
3	11.819 / 02 / 2012	J. Guarro	D = 0.41 m	LHIRES III 1200 l/mm	Atik314L+	4500 s	5000	6425 - 6760	_suaur_20120211_819_guarro.fit
4	12.766 / 04 / 2012	C. Buil	D = 0.28 m (C11)	LHIRES III 600 l/mm	Atik314L+	11 x 600 s	3400	6160 - 6860	_suaur_20120212_766_buil.fit
5	12.824 / 02 / 2012	J. Guarro	D = 0.41 m	LHIRES III 1200 l/mm	Atik314L+	4500 s	5000	6145 - 6760	_suaur_20120212_824_guarro.fit
6	13.842 / 02 / 2012	J. Guarro	D = 0.41 m	LHIRES III 1200 l/mm	Atik314L+	6000 s	5000	6145 - 6760	_suaur_20120213_842_guarro.fit
7	14.829 / 02 / 2012	J. Guarro	D = 0.41 m	LHIRES III 1200 l/mm	Atik314L+	5700 s	5000	6145 - 6760	_suaur_20120214_829_guarro.fit
8	15.849 / 02 / 2012	J. Guarro	D = 0.41 m	LHIRES III 1200 l/mm	Atik314L+	4500 s	5000	6145 - 6760	_suaur_20120215_849_guarro.fit
9	16.847 / 02 / 2012	J. Guarro	D = 0.41 m	LHIRES III 1200 l/mm	Atik314L+	4500 s	5000	6145 - 6760	_suaur_20120216_847_guarro.fit
10	17.805 / 02 / 2012	J. Guarro	D = 0.41 m	LHIRES III 1200 l/mm	Atik314L+	4500	5000	6145 - 6760	_suaur_20120217_805_guarro.fit
11	18.757 / 02 / 2012	C. Buil	D = 0.085 m (refrac.)	LHIRES III 600 l/mm	Atik314L+	8 x 600 s	4700	6160 - 6860	_suaur_20120218_757_buil.fit
12	18.838 / 02 / 2012	J. Guarro	D = 0.41 m	LHIRES III 1200 l/mm	Atik314L+	4500	5000	6145 - 6760	_suaur_20120218_838_guarro.fit
13	20.763 / 02 / 2012	C. Buil	D = 0.085 m (refrac.)	LHIRES III 600 l/mm	Atik314L+	10 x 600 s	4400	6160 - 6860	_suaur_20120220_763_buil.fit

Conditions for use of data in publications

Note there is no a complete validation check prior to adding spectra to this table. Users should verify the quality of the spectra with the observers concerned.
Use of these data in research publications is encouraged (with citation or association of observers concerned).

Plots

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