Historical Perspective Overview of Capabilities Early Science Examples The Submillimeter Array David J. Wilner (Harvard-Smithsonian CfA) & SMA Team

September 24, 2004ESO ALMA Community Day2 Key People SMA Director Jim Moran Project Scientist Paul Ho Receiver/Antenna Ray Blundell Technical Bob Wilson Operations (Hilo) Ant Schinckel ASIAA Sun Kwok The SMA is a collaborative project of the Smithsonian Astrophysical Observatory, part of the Harvard-Smithsonian Center for Astrophysics, and the Academia Sinica Institute of Astronomy and Astrophysics (Taiwan)

September 24, 2004ESO ALMA Community Day3 SMA Project Development 1984: SAO Study: –six 6 m antennas –subarcsecond resolution –high altitude site –receiver development 1992: SAO becomes antenna contractor 1994: OSDA U. Hawaii 1996: ASIAA expansion –add two antennas  eight 1998: fringes at Haystack : antennas deployed to Mauna Kea

September 24, 2004ESO ALMA Community Day4 Specifications Mauna Kea Submillimeter Valley 1998 SMA Dedication November 2003

September 24, 2004ESO ALMA Community Day5 Specifications Antennas: 8 antennas of 6 m diameter, 12  m rms surface cost + imaging speed + collecting area (~JCMT) Configurations: 24 pads in four rings baseline lengths m, subarcsecond resolution, best 0.1’’ Receivers: max 8 per antenna; 2 simultaneously (late 2004) full frequency coverage of atmospheric windows dual polarization; “high” & “low” for calibration GHz (8 in operation) GHz (8 in operation) GHz (start 2005), GHz (future) GHz (6 in operation, 2 soon) GHz (future) Correlator: 2 GHz bandwidth, 0.1 MHz resolution sensitivity, span/resolve extragalactic/galactic lines SMA Specifications (and drivers)

September 24, 2004ESO ALMA Community Day6 f/0.4, surface 72 aluminum panels, carbon fiber bus SMA Antennas 65  m12  m near-field holography GHz pointing rms 2” - 5” (night), improvements under study fast slews all weather

September 24, 2004ESO ALMA Community Day7 Array Configurations 4 tangent “rings” based on Reuleux Triangles (Keto ‘97) activate outer pads early 2005 JCMT/CSO link tests start 2005

September 24, 2004ESO ALMA Community Day8 Receiver Bands/Atmospheric Transmission 230 GHz345 GHz 690 GHz805 GHz 460 GHz

September 24, 2004ESO ALMA Community Day9 Receiver Performance (R. Blundell) 230 GHz 345 GHz 690 GHz Lab Field (ALMA)

September 24, 2004ESO ALMA Community Day10 Weather: CSO  225 for last two weeks

September 24, 2004ESO ALMA Community Day11 10 GHz LSB: 2 GHz = 24x82 MHz USB: 2 GHz = 24x82MHz Correlator e.g. Orion-KL, Beuther et al., in prep

September 24, 2004ESO ALMA Community Day12 Passband Visualization Tool

September 24, 2004ESO ALMA Community Day13 Beam Calculator/Sensitivity Estimator

September 24, 2004ESO ALMA Community Day14 Beam Calculator/Sensitivity Estimator

September 24, 2004ESO ALMA Community Day15 1. Solar System 2. Low-mass SF 3. High-mass SF Early Science Projects 4. Evolved Stars 5. Galactic Center 6. Galaxies 18 papers in press (astro-ph); ApJ Letters Special Issue

September 24, 2004ESO ALMA Community Day16 CO(3-2), HCN(4-3) and isotopes, other nitriles Titan (Gurwell)

September 24, 2004ESO ALMA Community Day17 most nearby protoplanetary disk at 56 pc (dec. -34) dust, CO J=3-2: disk structure, kinematics, M *, chemistry TW Hya (Qi et al.) 870  m dust 500 AU

September 24, 2004ESO ALMA Community Day18 binary protostar, 5” projected separation D=150 pc, L~20 L sun, common envelope “hot core” chemistry, e.g. C 2 H 3 CN, HCOOCH 3, T>100 K, n>10 6 cm -3 high resolution images show differentiation between the two cores IRAS16293 Chemistry (Kuan et al.) MM1 MM2

September 24, 2004ESO ALMA Community Day19 early example of collapse from redshifted absorption; controversial HCN J=4-3 traces high densities in envelope/outflow include JCMT short spacings inverse P-Cygni profile against dust continuum IRAS16293 Kinematics (Takakuwa et al.) HCN J-4-3 2’’ beam MM1 MM2

September 24, 2004ESO ALMA Community Day20 Orion-KL (Beuther et al.) nature of source “I” continuum emission: HII region + dust? or H- free free? first subarcsecond submillimeter image

September 24, 2004ESO ALMA Community Day21 Orion-KL (Beuther et al.) spectral line images! (no confusion at source I)

September 24, 2004ESO ALMA Community Day GHz H 2 O masers (Patel et al.) resolve two regions of maser emission in Ceph A

September 24, 2004ESO ALMA Community Day23 nearby AGB star with rich circumstellar chemistry first 690 GHz band image (3 antennas) IRC CS J=14-13 (Young et al.)

September 24, 2004ESO ALMA Community Day GHz emission likely originates from ~10 R S of SMBH (variability on range of timescales, see Zhao et al.) SgrA* Linear Pol. (Marrone et al.) I QU July 6, 2004 preliminary 6.7+/-0.5%, 171+/-2 deg small beam mitigates dust contamination to emission switching 1/4-wave plates

September 24, 2004ESO ALMA Community Day25 Isaac Newton Telescope INT-WFC 12 CO(2-1) SMA 5 Antenna Observation 12 CO(3-2) SMA 4 Antenna Observation Sakamoto et al. (1999 ) 810 pc 12 CO(1-0) NMA grand design spiral, D=8.4 Mpc M51 (Matsushita et al.) HST NMA nucleus warm (~100 K) and dense (~10 4 cm -3 ) AGN/Starburst activity

September 24, 2004ESO ALMA Community Day26 VV114 Interacting Galaxies (Iono et al.) OVRO CO 1-0 SMA CO 3-2SMA CO 2-1 CO J=2-1 in both galaxies and in overlap CO J=3-2 dense gas in VV114E velocity dispersion largest in overlap

September 24, 2004ESO ALMA Community Day27 science observations –5 nights per week (2 nights for engineering/commissioning) –typically ~50% suitable for 345 GHz band partner fractions: CfA:ASIAA:IfA = 72:13:15 –partners have independent time allocation procedures last CfA proposal deadline: Sep 16, 2004 for Nov-Apr –~ 50 proposals received; some very large time requests –up to 10% of CfA time to external PI’s with CfA collaboration –690 GHz band and long baselines internal for now next CfA deadline: Mar 2005; more time for visitors see for tools, forms, call Observing Time and Proposals

September 24, 2004ESO ALMA Community Day28 must be ready for the best weather! dual band operation will facilitate calibration more antennas  better self-calibration Prospects for 690 GHz Band IRAS16293 (5 antennas) use 658 GHz H 2 O masers?

September 24, 2004ESO ALMA Community Day : dual band operation  more 690 GHz 2005: activate outer pads  highest resolution 2005: JCMT-CSO link tests (“eSMA”) 2005+: receivers for GHz; dual pol GHz ???: receivers for 490 GHz and 805 GHz bands ???: more pads for > 500 m baselines ongoing calibration issues –improve pointing, esp. daytime –improve bandpass calibration (noise drawer) –phase correction tests (continuum, IRMA,183 GHz H 2 O line) SMA Development

September 24, 2004ESO ALMA Community Day30 first test of long baselines (pad 18) April GHz band atmospheric “seeing” can be very good, esp. at night CO J=3-2, resolve E-W double nucleus,  min = 0.36” Arp 220 (Sakamoto et al.)

September 24, 2004ESO ALMA Community Day31 SMA opens Submillimeter Interferometry for ALMA submm

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September 24, 2004ESO ALMA Community Day33 Historical Perspective: mid 1980’s –recognition that wavelengths mm observable from ground offer (unique) opportunities to study gas and dust –large single dish submillimeter telescopes under construction –pioneering millimeter interferometers starting operation JCMT 15m CSO 10m BIMA PdBI OVRO NMA &

September 24, 2004ESO ALMA Community Day34 invert spectrum to retrieve HCN abundance vs. altitude Titan (Gurwell)

September 24, 2004ESO ALMA Community Day35 first 8 antenna image, Nov 2003 CO J=2-1 emission and absorption plus thermal continuum diurnal temperature contrast Mars (Gurwell)

September 24, 2004ESO ALMA Community Day36 thermal emission from nucleus, chemistry of inner coma Comet in May 2004 (Qi et al.) 235 GHz continuum CS J=5-4 emission

September 24, 2004ESO ALMA Community Day37 M83 Morphology (Sakamoto et al.) face-on, barred spiral at 4.5 Mpc (1’’=22 pc) visible nucleus offset from center? 2.2  m (Thatte, Tecza, Genzel 1999) HST U,V,I composite (Harris et al. 2001) offset gas ridges + nuclear ring CO J=2-1, J=3-2

September 24, 2004ESO ALMA Community Day38 M83 Dynamics (Sakamoto et al.) CO velocities suggest center of symmetry ≈ dynamical center visible nucleus offset; high velocity gas, steep gradient  disk rotating around visible nucleus r ~ 40 pc, M dyn ~3  10 8 M Sun final stage of a minor meger; visible nucleus = remnant satellite core starburst arc, m=1 mode? visible nucleuscenter of symmetry

September 24, 2004ESO ALMA Community Day39 starburst fuel: 12 CO/ 13 CO/C 18 O J=2-1 surprising superbubbles (origin?) NGC 253 (Sakamoto et al.)

September 24, 2004ESO ALMA Community Day40 Debris Disks and High-z Galaxies Planet Signatures faint sources require full design performance Examples of Future SMA Targets Wilner et al., in prep Downes et al HDF850.1 PdBI CSO