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A Survey of Orion A with XMM and Spitzer: SOXS

Delve into the comprehensive survey of Orion A using XMM and Spitzer to study star formation, disk evolution, and X-ray impacts with detailed multi-wavelength observations.

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A Survey of Orion A with XMM and Spitzer: SOXS

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  1. A Survey of Orion A with XMM and Spitzer: SOXS Scott Wolk Harvard-Smithsonian Center for Astrophysics In collaboration with: Tom Megeath, Lori Allen, John Bally, Luisa Rebull Marc Gange, Guisi Micela, Salvo Sciortino, Lee Hartman, Fred Walter, John Stuaffer, Joanna Olivaria and Rob Gutermuth

  2. Goals for the SOXS Multi-wavelength observations are providing a wealth of information on the distribution and motions of stars, protostars, and cores in giant molecular clouds. These data are an essential constraint on models of the formation and evolution of clusters. Identify the PMS stars without disks - A full cluster census. Study the relative importance of clustered and isolated star formation. Examine the effect of environment on star formation and disk evolution. Study Transition disk timescales Effect of X-rays, especially flares on planet forming disks.

  3. Orion A CO/Optical map from CfA mm group

  4. Orion A Orion B • 105 M molecular cloud • One of the nearest regions of clustered star formation • One of the most active regions of distributed (i.e. isolated) star formation within 500 pc. Orion Nebula Orion A 13CO 2.6 mm Bally et al.

  5. 105 M molecular cloud • One of the nearest regions of clustered star formation. • One of the most active regions of distributed (i.e. isolated) star formation within 500 pc. Orion A

  6. The Spitzer Survey of Orion A • The Spitzer survey shows that the Orion Nebula Cluster is the most concentrated region of star formation in the cloud. • Spitzer found ~1000 young low mass stars with disks and protostars in the ONC.

  7. The Spitzer Survey of Orion A • In addition, the survey finds 700 young stars and 140 protostars south of the ONC. • These young stars are found in much different environment than that found in the ONC; either in small clusters of 10-50 stars or in relative isolation. • These stars have formed in environments without the strong UV radiation and dense clustering found in the ONC. A significant fraction of the stars are in a distributed component parsecs away from the massiveOB stars. Megeath et al. in prep.

  8. Nearest neighbor density Density = 10/p r2 r =distance to 9th nearest neighbor distributed clustered The Spitzer Survey of Orion A White contours: AV = 3 (Orion) Dots: young stars with IR-excess Colors other than green indicate clusters of more than 10. Megeath et al. in prep. There is no clear border between clustered and distributed stars Embedded clusters are not isolated, well defined objects

  9. By the Numbers • 1161 X-ray sources in the 9 fields • Nearly 100,000 IRAC sources in those fields. • About 140 Class I Sources in those fields • About 550 Class II sources are in the 9 fields. • About 220 (~45%) of the Class II sources were detected by XMM. • Of the 1161 X-ray sources, 882 have counterparts in the Spitzer Survey.

  10. Contaminationby Background X-ray Sources

  11. Filtering the Contaminants

  12. Colors of X-ray Sources

  13. L1641 S L1641S, the DL Ori group and the HBC 498 cluster R,G,B= 24,5.8, 3.6 m

  14. L1641 S

  15. L1641 N

  16. Stellar Content of Orion A • This is the total for the 9 fields. • It should be revised upward: • Minor incompleteness of IRAC. • Some incompleteness in cloud coverage in current XMM survey.

  17. Caveats • Need to really work field by field • Need to account for contamination from Orion 1A • Should be small • Examine influence of Ori.

  18. Status • Survey Completed March 2008 • Of the 1161 X-ray sources, 882 have counterparts in the Spitzer Survey. • About 563 have IRAC colors consistent with Class III sources • 99 have colors consistent with agn • 221 have colors consistent with CII. • The total number of stars in the 9 fields of Orion A is about 2100. • The Class III sources appear more dispersed than the Class II sources.

  19. Why Bother Looking at Young Stars in X-rays? • Young stars are X-ray bright • HMS- High energy wind shocks? • LMS- Despite pedestrian 5000K, temperatures they have hot corona. • Insight into the interior workings of LMS. • To identify young stars. • After stars lose their disks X-ray surveys are the only way to find young stellar objects • This has allowed us to understand the history of star formation in the galaxy. • Direct observation of material accreting onto very young stars. • X-rays are probably responsible for rapid heating of protoplanetary disks.

  20. COUP study of the ONC • 850 ks • 13 papers in the APJSupp • 465 refereed citations • 6 Refereed Papers since • XEST - 11 paper A&A special edition on Taurus SFR. • So aren’t we done?

  21. Orion AOB stars Orion B • 105 M molecular cloud • One of the nearest regions of clustered star formation • One of the most active regions of distributed (i.e. isolated) star formation within 500 pc. Orion Nebula Orion A 13CO 2.6 mm Bally et al.

  22. The Spitzer Survey of Orion A • The Spitzer survey shows that the Orion Nebula Cluster is the most concentrated region of star formation in the cloud. • Spitzer 1000 young low mass stars with disks and protostars in the ONC. L1641 N V 380 L1641 C HBC 498 L1641 S

  23. OB STARS

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