Á L V A R O S Á N C H E Z M O N G E B A R C E L O N A - N O V E M B E R 23, 2006 Centimeter and Millimeter Emission from Selected High-Mass Star-Forming.

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Á L V A R O S Á N C H E Z M O N G E B A R C E L O N A - N O V E M B E R 23, 2006 Centimeter and Millimeter Emission from Selected High-Mass Star-Forming Regions

ÁLVARO SÁNCHEZ MONGE - BARCELONA NOVEMBER 23, CENTIMETER AND MILLIMETER EMISSION FROM SELECTED HIGH-MASS STAR-FORMING REGIONS INTRODUCTION Isolated mode Typically, one star per core of dense gas Low-Mass Star-Forming Regions Clustered mode A group of stars in a single massive dense core Low-Mass Star-Forming Regions High-Mass Star-Forming Regions Our aim is to study YSOs forming in the surroundings of high-mass stars. We need to study the gas and dust condensations with: high-angular resolution. high sensitivity. STAR FORMATION

ÁLVARO SÁNCHEZ MONGE - BARCELONA NOVEMBER 23, CENTIMETER AND MILLIMETER EMISSION FROM SELECTED HIGH-MASS STAR-FORMING REGIONS SELECTION CRITERIA We need candidates to massive protostarsSelected from the lists compiled by Molinari et al (A&A, 308, 573) Mueller et al (ApJS, 143, 469) Sridharan et al (ApJ, 634, L57) Distance  3.5 kpc We want to study the surroundings of high-mass star-forming regions. IRAS bolometric luminosity  1000 L  Strong millimeter emission in single-dish (I 1.2 mm  100 mJy beam -1 ) Weak centimeter emission (S 3.6 cm  10 mJy) to be sensitive to low-mass condensations of  1 M  to select intermediate/high-mass targetsto assures a young evolutionary stage of the massive star-forming region to assures that the HII region is not evolved enough to have disrupted the surrounding material For 10 regions we found no available cm & mm data in the literature

ÁLVARO SÁNCHEZ MONGE - BARCELONA NOVEMBER 23, CENTIMETER AND MILLIMETER EMISSION FROM SELECTED HIGH-MASS STAR-FORMING REGIONS OBSERVATIONS IRAM 30m MPIfR 117-element bolometer array MAMBO we map the dust continuum emission at 1.2 mm VLA (Very Large Array) we observed the radio-continuum emisson at 3.6 and 1.3 cm

ÁLVARO SÁNCHEZ MONGE - BARCELONA NOVEMBER 23, CENTIMETER AND MILLIMETER EMISSION FROM SELECTED HIGH-MASS STAR-FORMING REGIONS RESULTS centimeter sources detected in the survey with the flux density at 3.6 and 1.3 cm we can estimate the spectral index  12 can be classified as HII regions physical parameters of the UCHII regions

ÁLVARO SÁNCHEZ MONGE - BARCELONA NOVEMBER 23, CENTIMETER AND MILLIMETER EMISSION FROM SELECTED HIGH-MASS STAR-FORMING REGIONS YOUNG CLUSTERS centimeter compact sources millimeter emission 2MASS source with small infrared excess Young Cluster * * Klein et al (ApJSS, 161, 361)

ÁLVARO SÁNCHEZ MONGE - BARCELONA NOVEMBER 23, CENTIMETER AND MILLIMETER EMISSION FROM SELECTED HIGH-MASS STAR-FORMING REGIONS IRAS L = 1300 L  d = 1.8 kpc Spectral index (VLA 2+3): 0.5 ± 0.2 Spectral type: B 2 M dust = 40 M  NH 3 detected Black:3.6 cm White:1.3 cm Green:1.2 mm Crosses:2MASS sources Ellipse:IRAS ellipsoide Good Candidate to study interactions between YSOs

ÁLVARO SÁNCHEZ MONGE - BARCELONA NOVEMBER 23, CENTIMETER AND MILLIMETER EMISSION FROM SELECTED HIGH-MASS STAR-FORMING REGIONS IRAS L = 7900 L  d = 2.6 kpc Spectral index (VLA 2): 0.4 ± 0.3 Spectral type: B 1 M dust = 160 M  Black:3.6 cm White:1.3 cm Green:1.2 mm Crosses:2MASS sources Ellipse:IRAS ellipsoide

ÁLVARO SÁNCHEZ MONGE - BARCELONA NOVEMBER 23, CENTIMETER AND MILLIMETER EMISSION FROM SELECTED HIGH-MASS STAR-FORMING REGIONS IRAS L = 1600 L  d = 1.6 kpc Spectral index (VLA 8): 1.0 ± 0.3 Spectral type: B 2.5 M dust = 11 M  Black:3.6 cm White:1.3 cm Green:1.2 mm Crosses:2MASS sources Ellipse:IRAS ellipsoide

ÁLVARO SÁNCHEZ MONGE - BARCELONA NOVEMBER 23, CENTIMETER AND MILLIMETER EMISSION FROM SELECTED HIGH-MASS STAR-FORMING REGIONS EVOLVED PROTOCLUSTERS centimeter compact sources millimeter emission 2MASS source with high infrared excess Evolved ProtoCluster * * Klein et al (ApJSS, 161, 361)

ÁLVARO SÁNCHEZ MONGE - BARCELONA NOVEMBER 23, CENTIMETER AND MILLIMETER EMISSION FROM SELECTED HIGH-MASS STAR-FORMING REGIONS IRAS Spectral index (VLA 1): < 1.1 Spectral type: B 2.5 Black:3.6 cm White:1.3 cm Green:1.2 mm Crosses:2MASS sources Ellipse:IRAS ellipsoide L = 4000 L  d = 2.5 kpc M dust = 26 M  NH 3 detected

ÁLVARO SÁNCHEZ MONGE - BARCELONA NOVEMBER 23, CENTIMETER AND MILLIMETER EMISSION FROM SELECTED HIGH-MASS STAR-FORMING REGIONS NGC IRS 9 Spectral index (VLA 2): > -1.3 Spectral type: B 1 L = L  d = 2.8 kpc Spectral index (VLA 3): > -0.1 Black:3.6 cm White:1.3 cm Green:1.2 mm Crosses:2MASS sources Ellipse:IRAS ellipsoide Blue lines:outflows Spectral type: B 1.5 M dust = 40 M  NH 3 detected

ÁLVARO SÁNCHEZ MONGE - BARCELONA NOVEMBER 23, CENTIMETER AND MILLIMETER EMISSION FROM SELECTED HIGH-MASS STAR-FORMING REGIONS PROTOCLUSTERS centimeter compact sources millimeter emission no 2MASS source associated ProtoCluster * * Klein et al (ApJSS, 161, 361)

ÁLVARO SÁNCHEZ MONGE - BARCELONA NOVEMBER 23, CENTIMETER AND MILLIMETER EMISSION FROM SELECTED HIGH-MASS STAR-FORMING REGIONS IRAS L = 1300 L  d = 1.3 kpc Spectral index (VLA 3): 1.3 ± 0.4 Spectral type: B 3 M dust = 25 M  NH 3 detected Black:3.6 cm White:1.3 cm Green:1.2 mm Crosses:2MASS sources Ellipse:IRAS ellipsoide The Youngest Massive Star of this Survey

ÁLVARO SÁNCHEZ MONGE - BARCELONA NOVEMBER 23, CENTIMETER AND MILLIMETER EMISSION FROM SELECTED HIGH-MASS STAR-FORMING REGIONS “EXTRA” centimeter emission displaced with respect to the millimeter emission no 2MASS associated “Extra”

ÁLVARO SÁNCHEZ MONGE - BARCELONA NOVEMBER 23, CENTIMETER AND MILLIMETER EMISSION FROM SELECTED HIGH-MASS STAR-FORMING REGIONS “EXTRA” (1) IRAS IRAS no 2MASS source millimeter emission displaced no 2MASS source millimeter emission displaced extended emission

ÁLVARO SÁNCHEZ MONGE - BARCELONA NOVEMBER 23, CENTIMETER AND MILLIMETER EMISSION FROM SELECTED HIGH-MASS STAR-FORMING REGIONS “EXTRA” (2) IRAS IRAS cluster of 2MASS sources millimeter emission displaced extended emission no 2MASS source millimeter emission displaced 3.6 cm emission displaced 1.3 cm emission displaced

ÁLVARO SÁNCHEZ MONGE - BARCELONA NOVEMBER 23, CENTIMETER AND MILLIMETER EMISSION FROM SELECTED HIGH-MASS STAR-FORMING REGIONS SUMMARY We have studied 10 regions at mm & cm wavelengths We have found 12 HII regions, most of them UCHII regions In all the cases, a B type star is required to ionize the gas We can classify the UCHII regions in different evolutionary stages IRAS is a good candidate to study the surrounding material (a complete study of this source will be presented in Busquet et al.)

Á L V A R O S Á N C H E Z M O N G E B A R C E L O N A - N O V E M B E R 23, 2006 Thank You ! Centimeter and Millimeter Emission from Selected High-Mass Star-Forming Regions