1. Name: Structure and starformation of LMC/SMC molecular clouds Authors: Aalto, Johansson, Rubio, Tatematsu, Black, Viallefond(?) 2. Science goal: The Magellanic Clouds provide unique possibilities to study the effects of metallicity and radiation field on the structure of the the interstellar medium (ISM). For example, there is tentative evidence that the interstellar molecular gas in the Magellanic Clouds is characterized by a higher degree of clumping than is the case in the Galaxy. This is suggested to be an effect of reduced dust abundances and, accordingly, a deeper penetration of the UV radiation into the ISM, producing strong photodissociation of the molecular species. So far, SEST has provide the highest resolution observations, 10 pc, barely enough to resolve giant molecular clouds (GMC's) in these galaxies. Thus, to establish the true structure of the molecular clouds it is fundamental to study the molecular gas in the LMC/SMC at considerably higher resolution, i.e., 0.1 pc or even less. We suggest observations of a sample of molecular clouds in the LMC and the SMC, i.e., galaxies of significantly different metallicities. Within each galaxy, regions of different radiative environments should be observed. This strategy has the prospect to separate the impact of the metallicity and the radiation field on the structure of the clouds. With a resolution of 0.2 arcseconds we reach linear scales of 0.05 pc. The Magellanic clouds provide a star formation environment which is different in many aspects from that of the Galaxy. It is likely that some of the aspects of starformation in this low metallicity environment are similar to those in the early universe. Due to lack of resolution it has not been possible to study the properties of the newly formed stars in any detail in the LMC. The high angular resolution provided by ALMA will allow us detection of bipolar outflows from young massive stars embedded in the MCs - in particular in the 30DOR region. 3. Number of sources: two clouds in 30DOR, three in N159; two in SMC 4. Coordinates: 4.1. 30 Doradus and N159, LMC (RA=05h40m, DEC=-69d) SMC (RA=01h, DEC=-73d) Two MC in LMC one in 30DOR (intense radiation field) the other N159 in more quiescent surroundings. 4.2. Moving target: no 4.3. Time critical: no 5. Spatial scales: 5.1. Angular resolution: 1" - 0.2" (0.2" for a few pointings) 0.2"=0.05 pc linear 5.2. Range of spatial scales/FOV: At 230 GHz (Band 6) the field-of-view is about 35" 5.3. Single dish: yes (already existing) 5.4. ACA: yes 5.5. Subarrays: no 6. Frequencies: 6.1. Receiver band: Band 6: 211 - 275 GHz 6.2. Lines: CO 2-1 fov: 30 arcsec Frequency: 230 GHz 6.3. Spectral resolution (km/s): 0.2 km/s 6.4. Spectral coverage (km/s or GHz): 20 km/s 7. Continuum flux density: (not applicable) 7.1. Typical value: 7.2. Continuum peak value: 7.3. Required continuum rms: 7.4. Dynamic range in image: 8. Line intensity: 8.1. Typical value: 5-10 K 8.2. Required rms per channel: 0.5 K 8.3. Spectral dynamic range: 20 ? 9. Polarization: no 10. Integration time per setting: 50 hrs survey plus 120 hrs high res mode= 170 hrs Survey mode - 1", 0.2 km/s resolution at 230 GHz (sensitivity 0.1 K after 20 minutes): CO 2-1 fov 35": 30DOR: 2x16= 32 pointings to cover two MCs in 30 DOR times 20 minutes = 10 hrs N159: 3x16 = 48 pointings to cover three clouds = 15 hrs Double this time to cover similar regions in the SMC = 25 hrs High res mode - 0.2", 0.1 km/s resolution 230 GHz (sensitivity 0.5 K after 10 hours): 30DOR: two pointings in one cloud: central and outskirt - 10 hours per pointing N159: two pointings in two clouds - N159W and N159S A total of 60 hours Same distribution in SMC = 60 hours. 11. Total integration time for program: 170 hr **************************************************************************** Review Christine Wilson: interesting program, looks OK to me Integration time not checked.