Instruments we may need or may not

Armagh, 19 February 2008 This session:  MuSiCoS, Narval & ESPaDONs archive (James)  DAO (Jason)  Archive observations (Luca)

Armagh, 19 February 2008 Part I The most obvious choices  Optical spectroscopy and spectropolarimetry

Armagh, 19 February 2008 High resolution spectropolarimetry Pic-du-Midi

Armagh, 19 February 2008 High resolution spectropolarimetry CHFT

Armagh, 19 February 2008 High resolution spectropolarimetry DAO

Armagh, 19 February 2008 High resolution spectropolarimetry ESO?

Armagh, 19 February 2008 Low resolution spectropolarimetry ESO)

Armagh, 19 February 2008 Low resolution spectropolarimetry

Armagh, 19 February 2008 V/I = x 10 –13 2 dI/d 1/I + V 0 /I 0 = /- 150 G

Armagh, 19 February 2008 Low resolution spectropolarimetry WHT)

Armagh, 19 February 2008 Low resolution spectropolarimetry SALT?

Armagh, 19 February 2008 Low res. spectropolarimetry: Advantages and drawbacks  Extremely efficient on hot and fast rotating stars  No additional use other than for field determinations

Armagh, 19 February 2008 High resolution spectroscopy:

Armagh, 19 February 2008 High resolution spectroscopy: NOT

Armagh, 19 February 2008

Armagh, 19 February 2008 High resolution spectroscopy VLT)

Armagh, 19 February 2008 High/mid-to-low resolution multi- object spectroscopy:

Armagh, 19 February 2008 High/mid-to-low resolution multi- object spectroscopy:

Armagh, 19 February 2008 High/mid-to-low resolution multi- object spectroscopy:

Armagh, 19 February 2008 FLAMES Fiber Large Array Multi-Element Spectrograph 132 GIRAFFE Medusa buttons 30 GIRAFFE IFU buttons 8 UVES buttons

Armagh, 19 February 2008 FLAMES Fiber Large Array Multi-Element Spectrograph NAME min (Ǻ) min (Ǻ) max (Ǻ) max (Ǻ)  (Ǻ) (Ǻ) (Ǻ) (Ǻ)R H H …………… H …………… H FLAMES high resolution settings

Armagh, 19 February 2008 FLAMES Fiber Large Array Multi-Element Spectrograph NAME min (Ǻ) min (Ǻ) max (Ǻ) max (Ǻ)  (Ǻ) (Ǻ) (Ǻ) (Ǻ)R L L …………… L …………… L FLAMES low resolution settings

Armagh, 19 February 2008 From less obvious to exotic  Photometry  Multi-objects vs. 3D spectroscopy  IR Imaging and spectroscopy  Interferometry  Radio  X-rays, UV  Astrometry (Gaia)

Armagh, 19 February 2008 REM

Armagh, 19 February D spectroscopy  Are we interested?

Armagh, 19 February 2008 NIR high resolution spectroscopy: VLT  R=100,000  Spectral coverage = 5 nm!

Armagh, 19 February 2008 Future instruments:  Spectral coverage: 0.9 to 2.5  m  Spectral resolution: R=50,000  15% throughput  S/N ratio = 100 with 1h exp on a J=13 star  Commissioning on 2013

Armagh, 19 February 2008 TNG  Similar to Spirou  Commissioning in 2009  Attached at the Nasmith

Armagh, 19 February 2008 High resolution NIR imaging  FWHM < 0.05” in JHK