1. SOME IMPLICATIONS FOR FUTURE CoRoT POINTINGS
GROUND-BASED OBSERVATIONS OF COROT SEISMO TARGETS
Ennio PORETTI (INAF-OA Brera) – Action SC 42- 1a
SOME IMPLICATIONS FOR FUTURE CoRoT POINTINGS
Need for good seismic targets expected to show clear line profile variations.
In absence of them, very difficult to re-submit a new LP supporting the CoRoT
second extension.
Radial velocity measurements of (sub)giants are not a self-consistent project.
With the length of HARPS runs, we can just obtain RV amplitude and nu_max.
Quite impossible to measure separations.
Radial velocity measurements of dwarfs would require short cadence spectra.
Since it is a must to observe many stars for the LP scientific profile, the observation
of just one (bright!) target weakens the proposal. Moreover, still limited access to
physical info, amplitude and nu_max only.
Next observing runs: July 3-13 and July Around the expected eclipse
of HD (July 20).
Last observing runs: in December 2012 and January 2013 (not scheduled yet).

2. First light HARPS-N at TNG, March 25, 2012.
Commissioning time started on April 12.

3. LONG TERM PROGRAMME (FOUR SEMESTERS)
SUBMITTED TO TELESCOPIO NAZIONALE GALILEO
(Canary Islands), NOW EQUIPPED WITH HARPS-N
PI and CoIs : E. Poretti, M. Rainer, F. Borsa, C. Maceroni,
M. Marconi, V. Ripepi, C. Aerts, P. Amado,
P. Mathias, A. Miglio, J. Montalban, C. Neiner.
10 consecutive nights (90 hours) in Visitor Mode
Problems with the target list:
HD (LPV already observed), HD 47219,
HD (solar-like star with planet), and
HD (Be, but faint)
If accepted, two HARPSs looking at the same targets in Dec
But, high-pressure expected on HARPS-N. E.g., 50 nights are
requested by the new GLOBAL ARCHITECTURES OF PLANETARY SYSTEMS (GAPS) team to study exoplanets

4. STARS SHOWING CLEAR LINE PROFILE VARIATIONS
Action SC 42- 1a
STARS SHOWING CLEAR LINE PROFILE VARIATIONS
RELATED WITH SCIENCE OF THE SECOND EXTENSION
Topic : HOT B SUPERGIANT SEISMOLOGY
HD V= B1 Ib
Topic: BETA CEPHEI VARIABILITY
V2052 Oph=HD V=5.83 B2 IV-V
Topic : New Be stars
HD V= B0.5 IV
HD V= B0 V
HD V= B2Ve

5. STARS SHOWING CLEAR LINE PROFILE VARIATIONS
Topic: RED GIANT VARIABLES WITH KNOWN PARALLAXES
HD 43023=HIP V=5.84 G8III nu_max=100 microHz
Challenging for first detection of LPV (v sini =4 km/s)
HD =HIP V= nu_max=45 microHz
Topic: DSCT VARIABLES Hot border Instability strip
HD V= A0 V.
Topic: GAMMA DOR VARIABLES
HD V=7.36 F5 Bona-fide

6. Suggestions:
Select an outstanding target in the Center direction in 2013
GOAL: to provide a bright scientific case to support LP proposal
(submission due in September 2012)
V2052 Oph=HD V= Beta Cep
HD V= Be
HD =HIP V= Red giant
HD V= DSCT+Abundances
HD V= Bona-fide GDOR
Fields to be validated in terms of secondary targets and exoplanetary field
Still unexplored: sinergies with the central stars of planetary systems.
To be tested with HD ?