Observability of YSOs with the WISE and AKARI

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

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 μm • IRC: 9 and 18 μm • FIS: 65, 90, 140 and 160 μm

WISE - Wide-field Infrared Survey Explorer Band centers 3. 4, 4. 6, 12 & 22 microns Sensitivity: 78, 108, 850 & 5200 micro. Jy Angular Resolution: 6, 6, 6 & 12 arc-seconds Position accuracy better than 0. 5 arc-seconds with respect to 2 MASS 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

Figure by Mc. Caughrean

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

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

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

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)

Model parameters

Grid of YSO SED models • ~20. 000 RT models • Large range of stellar masses (0. 1 – 50 MSol) 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)

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

r 1 I ~ r-2 r 2 A=1. 086 τ

Selective extinction

Observability of LDN 1551 NE

Observability of CI Tau

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

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

Class II • whole range: AKARI + WISE 3. 4 and 4. 6 μm • WISE 12 and 22 μm: Whitney et al. (2003)

Class III • Whole range: 3. 4, 4. 6 μm • 12, 65 and 90 μm: Whitney et al. (2003)

Summary & Plans • • Th a Detailedninvestigation for IR point sources in TAPO k yo and observability for YSOs Physical parameters uonf different wavelengths for typical YSO Observability range or classes -> what kind of YSOs can wey wait from the catalogs o ur. YSO clusters -> what can we see from theortical att Investigation for typical YSO classes with: en tio – various inclination n! – different models – mass, temperature, etc. • Connection between intensities / colors and parameters