1. Observability of YSOs with the WISE and AKARI infrared observatories Sarolta Zahorecz Eötvös University, Budapest PhD student, 3. year Thesis advisor: Dr. L. Viktor Tóth

2. AKARI Second Japan infrared astronomical satellite 68.5 cm diameter telescope two main instruments: – the Infrared Camera (IRC) – for mid-IR – the Far-Infrared Surveyor (FIS) – for FIR launched in February 2006 16 month cryogenic mission lifetime between May 2006 and August 2007 6 IR bands from 9 to 180 μ m IRC: 9 and 18 μ m FIS: 65, 90, 140 and 160 μ m

3. WISE - Wide-field Infrared Survey Explorer Band centers 3.4, 4.6, 12 & 22 microns Sensitivity: 78, 108, 850 & 5200 microJy Angular Resolution: 6, 6, 6 & 12 arc-seconds Position accuracy better than 0.5 arc-seconds with respect to 2MASS reference frame Data products include image atlas and point source catalog Over 1 million images covering the whole sky in 4 infrared wavelengths Catalogs of  500 million objects seen in these 4 wavelengths wise.astro.ucla.edu

5. Figure by McCaughrean

6. Observations of YSOs AKARI IRC + FIS WISE Other data from VizieR: USNO, 2MASS, Spitzer, IRAS, submm

7. SED Fitting Tool http://www.astro.wisc.edu/protostars We need: – Photometric data – A v range – Distance range We get: – Best fitting model, distance, A v

8. Developed by Whitney et al. (2003) Monte-Carlo radiation transfer code Computes SEDs, images, polarization maps Computed SEDs: – Inclination from 0° (polar view) to 90° (edge on) Stellar flux Disk flux Envelope flux The Radiation Transfer Code

9. YSO model Pre-main sequence star Disk Infalling envelope Bipolar cavities 14 parameters: Not all important at all stages of evolution Robitaille et al. (2006)

10. Model parameters

11. Grid of YSO SED models ~ 20.000 RT models Large range of stellar masses (0.1 – 50 M Sol ) and evolutionary stages (embedded protostars to dispersing disks) Parameters based on previous observations, predictions 10 different viewing angles for each SED -> ~ 200.000 SEDs Robitaille et al. (2006)

12. Observed and fitted sample SEDs Investigated regions: Taurus-Aurigra-Persues Orion Cold cloud cores from Planck/Herschel Galactic Cold Cores Key Project

13. I ~ r -2 r1r1 r2r2 A=1.086 τ

14. Selective extinction

15. Observability of LDN1551 NE

16. Observability of CI Tau

17. Class 0 only with AKARI whole range Whitney et al. (2003)

18. Class I WISE and AKARI: observable – AKARI: whole range – WISE: Whitney et al. (2003)

19. Class II whole range: AKARI + WISE 3.4 and 4.6 μm WISE 12 and 22 μm: Whitney et al. (2003)

20. Class III Whole range: 3.4, 4.6 μm 12, 65 and 90 μm: Whitney et al. (2003)

21. Summary & Plans Detailed investigation for IR point sources in TAPO Physical parameters and observability for YSOs Observability range on different wavelengths for typical YSO classes -> what kind of YSOs can we wait from the catalogs -> what can we see from theortical YSO clusters Investigation for typical YSO classes with: – various inclination – different models – mass, temperature, etc. Connection between intensities / colors and parameters