Access to large FoV for characterization of stellar population. Application to:

Extrasolar Planets Extrasolar Planets & &

Star Formation Star Formation

Isabella Pagano1

on behalf of J. Alcalà2, S. Benatti3, R. Claudi4, E. Covino2, S. Desidera4, D. Gandolfi5, A.F. Lanza1, A.C. Lanzafame6,

G. Leto1, S. Messina1, G. Piotto7, L. Spezzi8

Prospettive scientifiche per spettroscopia a grande campoINAF – Dipartimento progetti - Roma, 22 Ottobre 2008

1. INAF OACT, 2.INAF OACA, 3. CISAS. Univ. PD, 4. INAF OAPD, 5. Thüringer Landessternwarte Tautenburg, 6. Dip. Fis. & Astron. Univ. CT, 7. Dip. Astron. Univ. PD, 8. ESA/ESTEC

Extrasolar PlanetsExtrasolar Planets

• Search of transiting extrasolar planets requires high precision S/N photometry BS large fields in order to enhance the detection probability.

• Several projects on going:– Ground based, i.e.,

• SUPER WASP (64 sqr deg)

– Space based, i.e.:• CoRoT (2 sqr deg), Kepler (105 sqr deg),

PLATO (≥550 sqr deg)

Roma, 22 Oct 2008 I. Pagano - INAF OACT

Why large fields are desirableWhy large fields are desirable

Extrasolar PlanetsExtrasolar Planets

• Fast spectral characterization of targets in the chosen fields (low res spectroscopy, R≈2000-5000)

• Detection of binaries (R≥7000, i.e. 2-3 km s-1

in a selected spectral range)• Detection of activity level and age indicators:

Li 671 nm (R≥4000), H-alpha (R≥1000), Ca IRT(R≥8000)

Roma, 22 Oct 2008

Possible driversPossible drivers

H-alpha R ≈2000Medhi et al. 2007

Star FormationStar Formation

• Young molecular clouds, like Perseus, Serpens, Ophiucus are tenths of sqr-degree extended in the sky with a sparse stellar population of about 300-400 objects.

• A big effort to get IR/submm data is ongoing (Spitzer and the coming Herschel) for these Gould's Belt SFRs. This effort will allow to study star formation from the compact cores to debris disks. See next slide

• Optical Spectroscopy is the mandatory complement to assess the nature of the objects:• Li 671 nm & Halpha• Temperature, Mass

• Data from optical spectroscopy allow one to study the relation between stellar and disk parameters and to asses if there are preferred stellar masses for planet formation. See slide “stellar parameters”

Roma, 22 Oct 2008 I. Pagano - INAF OACT

IntroductionIntroduction

Star FormationStar Formation

Optical spectra have been obtained in few cases up to date, only for bright objects and young clusters that are a small fraction of these SFRs (e.g., IC348 in Perseus, Luhman et al. 2005; Upper Scorpius OB association, Preibish et al. 2001).

FLAMES has been used for these studies but: 25 arcmin FoV to cover wide SFRs like Perseus or Serpens weeks of

observing time would be needed (sparse stellar population) the sub-stellar population (I<18-18.5) is missed. You need to go deeper.

FORS feasible for some BDs, but field is small. VIMOS assures a larger FoV but R <≈19, not enough for most BDs

A 3x3 deg multi-objects (≈1000) spectrometer is desirable for these studies. It could be possible to cover a region like Perseus in 3-4 observing nights.

If imaging is also possible, such an instrument would be highly qualified (i.e., SED, extintion, disk parameters).

Roma, 22 Oct 2008 I. Pagano - INAF OACT

Why large fields are desirableWhy large fields are desirable

Star FormationStar Formation

• To study YSOs, BDs and free floating planets Li 671 nm (R ≥ 4000) and Halpha (R ≥1000) are really important: • membership, • accretion rates

• TiO & V bands (R ≥1000) to determine spectral type of small mass objects

• Ca IRT (R ≥8000) to have information on their magnetic activity.

Roma, 22 Oct 2008 I. Pagano - INAF OACT

Possible driversPossible drivers

Li 671nmR≈4000Preibisch et al. 2001

• Please GO ON!!!!

Thanks

Roma, 22 Oct 2008 I. Pagano - INAF OACT

3 × 3 deg

Spitzer IR-excess YSOs

Stellar parametersStellar parameters

Spectral Type Teff AV Aλ F0(λ)

L STAR

L DISK / ENVELOPE