PFS Observations of Galactic Objects2010.09.10Yoichi Itoh, Kobe University1/36Star Forming RegionsOpen ClustersHigh Resolution Mode

Luminosity function of nearby main-sequencesMass-Luminosity RelationPresent Day Mass Function Divide by ageInitial Mass Function

ProsCons1-1. Initial Mass Function11/36Salpeter (1955)

ProsIMFConsDistantBinary contaminationOptically faint due to interstellar extinction Obs. in near-infrared1-2. IMF of Star Forming Regions11/36Muench+ 2000Mass function of pre-main sequence stars (PMSs) in the Trapezium cluster

1-3. Imaging of Star Forming RegionsPseudo near-infrared map of the central region of NGC1333 (Oasa et al. 2008). Green circles are targets of spectroscopic obs.7/45Low mass SFRNearest : 140pcSolar-mass stars are born Taurus, Oph, PerseusMassive SFRNearest : 450pcOB starsOrion

Near-infrared imaging of central 5 x 5 region of NGC 1333 (Perseus, UH88)76 objects detected

Distinguish protostars and classical T Tauri stars from background stars by thermal radiation from envelopes and circumstellar disks.Near-infrared observations are efficient.Cannot identify WTTSs and half of CTTSs.1-4. YSOs or Backgrounds11/36weak lineT Tauri starprotoplanet44 PMSs identified

1-5. Spectroscopy of Pre-main SequencesH emission at 6563indicative of youthBroad TiO & VO abs. bandindicative of low temp.Determine spectral type from the band strengths (uncertainty : 1 subclass)

Not multi-object spectrograph.Only 14 objects were observed in one night.

10/45R-magnitudes : 14mag to 20magIUCAA 2m+IFOSCwavelengths520010300resolution14integration20 min to 120 min

Spectral type in the dwarf scale = lowest TeffSpectral type in the giant scale = highest TeffExtinction corrected J-mag = Boloemtric luminosity

Mass : 0.1Mo0.6Mo.2 young brown dwarfs?Age : 1Myr to10Myr

14(Itoh et al. 2010)

: Class I: Class II: Class III

1-6. Mass and Age of Pre-main Sequences16/45

HR

()1-7. Photometry or Spectroscopy11/36Luhman+ 2000dashedobjects with spectroscopysolidobjects with photometry

1-8. PFS Obs. of Star Forming Regionsred crossYSOsblue dotvisible stars

Only 100 YSOsYSOs are not widely distributed.Cloud is not extended

FMOS is sufficient.10/45NGC1333 (Perseus cloud). FOV=1.4

1-8. PFS Obs. of Star Forming RegionsPFSYSO1005000

R

HSCPFS : 1600nm-900nm

10/45TaurusTrapeziumSerpens

2. Open ClustersCluster membershipProper motion (Probability)Radial velocity (Probability)Spectral type (HR diagram)Pleiades : 2000

10/45(Diameter > 70, member candidates > 50 obj.) 9 clustersIntegration time : < 30 minutesWavelengths : 500nm-900nm?

3. Age of YSOs Giant()YSO()Dwarf ()Takagi et al. (2010)

()(R=20000)

4. Metallicity of Cluster Members

Funayama et al. (2009)

5. Summary SuMIRe = Subaru Multi-object Infra-Red Echellograph

Number of ObjectsFOVWavelengthStar Forming RegionsFMOSFMOSFMOSOpen ClustersFMOS/PFSPFSPFS

5-1.:?: S1063(Oasa+ 2008)

5-2. :? BRC14: BRC14()()C,B,A(Matsuyanagi+ 2006)

28/36

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