ALMA During Early Science

1. ALMA During Early Science National Radio Astronomy Observatory - NAASC Charlottesville, Virginia

2. The Breadth of ALMA Science ALMA • Image the redshifted dust continuum emission from evolving galaxies at epochs of formation as early as z = 10. • Probe the cold dust and molecular gas of nearby galaxies, allowing detailed studies of the interstellar medium in different galactic environments, the effect of the physical conditions on the local star formation history, and galactic structure. • Reveal the details of how stars form from the gravitational collapse of dense cores in molecular clouds. The spatial resolution of ALMA will allow the accretion of cloud material onto an accretion disk to be imaged, and will trace the formation and evolution of disks and jets in young protostellar systems. For older protostars and pre-main sequence stars, ALMA will show how (proto)planets sweep gaps in circumstellar and debris disks. • Uncover the chemical composition of the molecular gas surrounding young stars, including establishing the role of the freeze-out of gas-phase species onto grains, the re-release of these species back into the gas phase in the warm inner regions of circumstellar disks, and the formation of complex organic molecules • Image the formation of molecules and dust grains in the circumstellar shells and envelopes of evolved stars, novae, and supernovae. • Refine dynamical and chemical models of the atmospheres of planets in our own Solar System, and provide unobscured images of cometary nuclei, hundreds of asteroids, Centaurs, and Kuiper Belt Objects.

3. Cycle 0 ALMA • Sixteen 12m Antennae • Four Bands in the frequency range 84-720 GHz • A Compact Configuration, with a min/max baseline of ~18m/125m (largest observable scale ~ 21” at 100 GHz) • An Extended Configuration, with a min/max baseline of ~36m/400m (max angular resolution ~ 0.23” at 675 GHz) • Single pointing + mosaics (up to 50 pointings) • a number of spectral/continuum correlator modes, with bandwidths from 58.6 MHz and 2 GHz per baseband • Sources as far North as declination ~ 40o can be observed • Observations of moving targets (except the Sun) supported

4. Cycle 0 ALMA Observing Frequencies ALMA

5. ALMA Bands & Atmospheric Transmission ALMA 0.5mm pwv 1.3mm pwv Cycle 0 Bands • Resolution increases with increasing frequency • Weather (& sensitivity) degrade with increasing frequency

6. Example Correlator Modes ALMA Arp 220 HCN HNC HCO+ C2H 2 windows E.g., for Mode 7: ~6600 km/s bandwidth per spectral window (x 2 windows ) ~2 km/s resolution Dual polarization cuts the needed integration time in half.

7. Comparison with existing arrays ALMA

8. Spectral Coverage SMA CARMA IRAM PdBI ALMA Early Science 10 9 3 4 6 7 8 Comparison with existing arrays ALMA Collecting Area & Number of Baselines 8 (28) 23 (253) 64 (2016) 16 (120) 6 (15) (from D. Wilner)

9. ALMA test Data (5-6 Ant) ALMA Hot core of G34.26+0.15: at 3mm - lots of molecular lines detected in 2 hours.

10. ALMA Data ALMA β Pictoris disk: Herschel on left and 870 micron dust emission from ALMA

11. ALMA Data ALMA NGC 253: Band 6: CO (2→1) and Band 9: Continuum + CO(6→5)

12. ALMA Data ALMA BRI 0952-0115: (z =4.43) Ionized Carbon (CII @ rest-frame158 μm) detected in 1 hour

13. Cycle 0 ALMA • Call for Proposals issued 31 March 2011 • Proposal Deadline = 15:00 UT on 30 June 2011 • 500-700 hours of observations in Cycle 0 • North American time = 33.75% • Proposal Types: Standard (≤100 hours) & Target of Opportunity • Think of science that can be done in a few hours of observing time

14. Phase I Tools ALMA • Observing Tool (OT) • SIMDATA • Sensitivity Calculator • Splatalogue Screenshot of the Proposal Preparation Tool

15. Phase I Tools ALMA • Observing Tool (OT) • SIMDATA • Sensitivity Calculator • Splatalogue

16. Phase I Tools ALMA • Observing Tool (OT) • SIMDATA • Sensitivity Calculator • Splatalogue Screenshot of Sensitivity Calculator in the OT

17. Phase I Tools ALMA • Observing Tool (OT) • SIMDATA • Sensitivity Calculator • Splatalogue Screenshot of Splatalogue

18. Proposal Checklist ALMA • Read relevant documentation (CfP Guide, Primer) • Create an ALMA account by registering at the Science Portal • Download the Observing Tool (OT) & related guides • Prepare the Science & Technical Cases (PDF file) • Prepare Science Goals (sources, frequency & correlator setup, integration times) within the OT • Make use of the Helpdesk & the Knowledgebase

19. NRAO User Support ALMA NRAO User Support

20. The North American ALMA Science Center ALMA • located in Charlottesville, VA • User support for proposal preparation & post-observation • Support user visits to NAASC • NRAO Page Charge Support • Organize ALMA workshops http://science.nrao.edu/alma/index.shtml

21. The North American ALMA Science Center ALMA NAASC Postdocs Manuel Aravena, Rachel Friesen, VioletteImpellizzeri, Brian Kent, Amy Kimball, NuriaMarcelino, Robin Pulliam

22. The Atacama Large Millimeter/sub-millimeter Array (ALMA), an international astronomy facility, is a partnership of Europe, North America and East Asia in cooperation with the Republic of Chile. ALMA is funded in Europe by the European Organization for Astronomical Research in the Southern Hemisphere (ESO), in North America by the U.S. National Science Foundation (NSF) in cooperation with the National Research Council of Canada (NRC) and the National Science Council of Taiwan (NSC) and in East Asia by the National Institutes of Natural Sciences (NINS) of Japan in cooperation with the Academia Sinica (AS) in Taiwan. ALMA construction and operations are led on behalf of Europe by ESO, on behalf of North America by the National Radio Astronomy Observatory (NRAO), which is managed by Associated Universities, Inc. (AUI) and on behalf of East Asia by the National Astronomical Observatory of Japan (NAOJ). The Joint ALMA Observatory (JAO) provides the unified leadership and management of the construction, commissioning and operation of ALMA.

23. Key Cycle 0 dates ALMA