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X-rays from star-forming regions : Stellar and Interstellar Studies with XMM (and Chandra)

X-rays from star-forming regions : Stellar and Interstellar Studies with XMM (and Chandra). Thierry Montmerle (Grenoble) with : Nicolas Grosso & Hideki Ozawa (Grenoble) Myha Vuong (Saclay), Eric Feigelson (Penn State). 1. Nearby star formation in clusters :

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X-rays from star-forming regions : Stellar and Interstellar Studies with XMM (and Chandra)

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  1. X-rays from star-forming regions :Stellar and Interstellar Studieswith XMM (and Chandra) Thierry Montmerle (Grenoble) with : Nicolas Grosso & Hideki Ozawa (Grenoble) Myha Vuong (Saclay), Eric Feigelson (Penn State)

  2. 1. Nearby star formation in clusters : Introduction : case of the r Oph cloud 2. EPIC results : Stellar studies data analysis comparison with Chandra 3. Interstellar studies : Metallicity of nearby star-forming clouds using X-ray absorption Outline

  3. 1. Introduction Looking towards and through molecular clouds

  4. ISOCAM Chandra ACIS XMM EPIC The r Oph cloud core in X-rays : Chandra (5+100 ksec) + XMM (25 ksec) fields

  5. Lyman disc. dust gas+dust Röntgen, 1895 AV(tX=1) UV EUV x107 Cloud optical ~ EX–2.5 C 1 surface N O IR X 10 medium XMM/Chandra 100 core 10 mm 1 mm 0.1 keV 1 keV 10 keV 2 mm 2 keV ™

  6. 2. XMM/EPICobservations of the r Oph cloud Comparison with Chandra

  7. The XMM view of the r Oph cloud core (Grosso, Ozawa, Montmerle et al. 2003)

  8. Cross-Identification of MOS1, MOS2, and PN sources 3 s + 1” ⇒　same source Several “binary” sources → caused by alignment ?

  9. Identification between MOS1 and 2MASS 3 s + 1” ⇒　same source

  10. Identification between MOS2 and 2MASS 3 s + 1” ⇒　same source

  11. Identification between PN and 2MASS 3 s + 1” ⇒　same source

  12. Position correction of the EPIC images Before correction After correction

  13. Position correction of the EPIC images Before correction After correction

  14. Source detection and Identification with ChandraX-ray sources (Chandra data from Imanishi et al. 2001)

  15. Identification with Infrared YSOs X-ray detection rate • Class I : 7/11 (protostars : envelopes) • Class II : 28/61 (T Tauri stars with disks) • Class III : 14/15 (diskless T Tauri stars) Classification by Bontemps et al. 2001

  16. Lx vs. Lbol • Weak correlation between Lbol and LX　　index : 0.11 • LX/Lbol　is not constant withLbol

  17. 3. Looking through the r Oph cloud First measurement of the metallicity of a molecular cloud (Vuong et al. 2003)

  18. IR sources

  19. X-rays (> 100 cts) => NH,X NIR to MIR => AJ

  20. NH,X : Cross-check between Chandra and XMM (3 sources) [~107 K]

  21. ? Galactic relation µ X-ray counts

  22. NH,X <=> Metallicity from X-ray absorption AJ => AV via RV <=> grain properties

  23. The wide FOV of XMM/EPIC allows to capture the essence of high-energy star formation in one single exposure; links with IR however necessary to understand the nature of the sources => X-ray properties evolve significantly from protostars (envelopes) to “old” T Tauri stars (without disk) Spectral properties (absorption up to very high values) may be used to probe the metallicity of molecular clouds -a specific property of X-rays Conclusions(among others)

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