ALMA Science Results

Fourth in a series… www.almasc2014.jp

Summary of External Galaxy Talks Al Wootten

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ALMA Science Results

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ALMA Science Results

Themes • ALMA’s sensitivity and directivity enable studies of nuclear regions of galaxies – Still difficult to disentangle inflow from outflow; in some cases motions were kinematically complex – One needs a better measure of mass—for most objects only a limit could be established – Excellent prospects for measuring BH masses dynamically

• ALMA’s broad spectral grasp enables parallel excitation analyses among up to ~40 species.

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ALMA Science Results

Revolution in Astronomy • Galaxies and Galactic Nuclei I – 9:45 - 10:15 (invited) Quantifying key components in galaxies using ALMA: molecular clouds, dust, outflows, and supermassive black holes • Kotaro Kohno, University of Tokyo – Star formation converts HI through molecules to stars; ALMA studies the intermediate step. – Feedback: spatially resolved sensitive imaging critical for understanding feedback; ALMA provides this. – Combined ALMA data with Nobeyama 45m for M83 image. – NGC1808 – Arp 220: 434 micron imaging with ALMA reveals fine structure of its two nuclei. West nucleus requires AGN owing to high luminosity surface density. – NGC5044 group.

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ALMA Science Results

• Kohno (cont) – Outflows and Inflows in galaxies—central kinematics. – N1433-Combes et al.. CO deviates from ordered rotation: an outflow. – NGC1566 shows no outflow. Many talks on feedback and outflow at this meeting. – Measuring supermassive black holes with ALMA. Kinematic signature within rotation curve. – Submm water maser lines offer promise for measuring central kinematics of galaxies (Hagiwara)

– 10:15 - 10:30 The ALMA view of the starburst in NGC 253 • Alberto Bolatto, University of Maryland – Nuclear starbursts thought to be especially important at z~1-2 in galaxies. What drives them? What quenches them? Nearby NGC253 offers a nearby example. Hot xray radn seen by Chandra. ALMA view? – CO at high velocities correlates with the Xray streamers. Narrow, very turbulent short lifetime molecular structures. – Streamer bases lie near expanding molecular shells which may initiate them. – Outflow likely greater than 9 Msun/yr--may be lost but may be recycled.

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ALMA Science Results

– 10:50 - 11:05 Radio jets clearing the way: watching feedback in action in the Seyfert galaxy IC 5063 • Raffaella Morganti, ASTRON, Kapteyn Institute – H2 imaged with VLT, broad component near the jet. ALMA: 100pc resolution in CO 2-1 wraps around radio continuum well. – Kinematics: Clear correspondence to disturbances along the jet, deviates from rotation curve. Model: jet expands in clumpy medium

– 11:05 - 11:20 How do you drive molecular outflows? ALMA’s view of AGN feedback in NGC 1266 • Timothy Davis, University of Hertfordshire – – – –

Form: heats hot gas in galactic halos to prevent cooling. OR direct: removes star forming ISM Is it photon driven or jet driven? N1266 is most gas-rich early type galaxy in local Universe. Alatalo: CO shows outflow 500 km/s. Losing gas >110 Msun/yr. Chemistry can distinguish the form of the driver.SiO strong: shocks? – Weak ionized lines. Outflow seems to be powered by a nascent AGN jet.

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ALMA Science Results

– 11:20 - 11:35 Ballistic molecular rain powers cold black hole feedback in a cool core brightest cluster galaxy • Grant Tremblay, Yale University – Thanks for making ALMA accessible to optical/Xray observers. – A2597: 10 Msun/yr. z=.08. Cool core brightest cluster galaxy. Molecular gas follows ionized gas. CO2-1 with ALMA shows 2E9Msun cool gas. See a molecular fountain--molecular bubbles inflated by jet, permeated by young stars. Material slowly returns along filaments. – Infalling gas seen which can power the fountain.

– 11:35 - 11:50 The molecular gas outflow of NGC 1068 imaged by ALMA • Santiago Garcia-Burillo, OAN-IGN – Outflow in ionized gas, also in molecular circumnuclear disk. Dense tracers imaged to r~2kpc at 20-35pc resolution. – Find an off centered 200pc ring around AGN/ Kinematics--rotation and streaming. Find a molecular outflow at the circumnuclear disk. – Half of mass in CND is involved in outflow driven by AGN feedback. star formation cannot drive this outflow. – Many species also imaged. – Radiation pressure on dust could drive the outflow. 7

ALMA Science Results

– 11:50 - 12:05 ALMA observations of a candidate molecular outflow in obscured quasar SDSS J1356+1026 • Ai-Lei Sun, Princeton University – Redshift z=.123. N nucleus a galaxy, S nucleus less. Radioquiet. ALMA provided resolutions to 0.77kpc. No CO at ionized outflow; gas is in N nucleus with 1kpc tidal arm, very broad line. – Velocity too high to be rotation--outflow? – Star formation rate 100K, l10Msun/yr, N(H2)>10^24 cm^-2 so only radio and submm radiation can escape. – How much radiation comes from star formation how much from active nuclei? Observe many spectral lines and compare them to probe excitation. – Species often optically thick. Multiband scans provide many lines. 175GHz scan of NGC4418. Similar beam from 85-360GHz, The galaxy has high silicate absorption at ten microns. Narrow molecular lines, radio quiet. » Lines provide 30% of flux » Reach line confusion limit quickly; fit whole spectrum at once. Lots of HC3N, also vib-excited variant. Also HC5N. 40 molecules – Vibrationally excited HCN, HNC, HC3N probe the 5pc size source at center. Temperatures vary >100K. A new chemistry? – Can fit 90% of emission from lines. 10

ALMA Science Results

– Distributions of molecules in the circumnuclear disk and surrounding starburst ring in the Seyfert galaxy NGC 1068 observed with ALMA • Shuro Takano: – NRO45m 3mm survey laid foundation for ALMA survey. N1068: Syf 2 nucleus. 14.4Mpc distance so 1”=72pc. Circumnuclear disk has two knots. – Selected spectral windows based on 45m data. In some lines, the ring dominates, in others the CND is also promonent. Astonishment no 1: Methanol differs in the ring from 13CO. Astonishment 2: Some complex species concentrate in CND where X-rays are strong: HNCO, CH3CN. Astonishment 3: Ten line distributions obtained with an hour time in Cycle 0

– 15:00 - 15:15 Diffuse and dense gas in nearby luminous merging galaxies • Toshiki Saito, University of Tokyo – Observed VV114, N3110, N1614 with ALMA. Some ALMA Cycle 2 results shown. – CO 6-5 is more compact than low J CO. – The CO 6-5 traces intense nuclear star formation. – Claims that shocked regions traced in CS and CH3OH lines.

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ALMA Science Results

– 14:45 - 15:00 ALMA explorations of warm dense molecular gas in nearby LIRGs • Kevin Xu, California Institute of Technology/IPAC – .4mm CO 6-5, continuum – How does warm gas distribute in LIRG nuclei » Correlate with star formation? Are outflows important? When do AGNs dominate heating of gas and dust? – NGC34 and NGC1614. Former has CO in unresolved core, warmer gas. AGN35 km/s/kpc. Fast shocks destroy gas. – HST data appears to show young clusters in center. Star formation and spurs are seen, undetected in CO. Dust is detected only in the star forming ring. – Kim Scott-Evolution of molecular gas fraction. CO 3-2 in star forming galaxies from COSMOS 100% detection rate. intermediate redshift. Complex line profiles. – Large mass-selected samples for fH2 evolution with redshift being observed in Cycle 2. Scoville, Scott, Sheth, Schinnerer.

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ALMA Science Results

– 16:35 - 16:50 ALMA and VLA measurements of frequencydependent time lags in Sgr A*: evidence for a relativistic outflow • Christiaan Brinkerink, IMAPP, Radboud University Nijmegen – What is SgrA* exactly?? Accretion flow? Jet? SED appears partially self-absorbed synchrotron. Usually this type has a jet. – Measured time lag in radio emission. Some part of jet is optically thick at some frequency. High frequencies closer in, see those first. – ALMA maps of the mini spiral dynamic range 4000 total time on source 6 mins. 3mm, 1mm, .8mm observed. Show varying spectrum. – More variation in flux at higher frequencies.What is the inclination angle? Use size measurements at high nu with VLB – Combine observations. Model them--can get moderately relativistic outflows--unresolved jet? Inclination still uncertain.

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ALMA Science Results

– 16:50 - 17:05 Ionized gas observations toward a nearby starburst galaxy NGC 253 • Kouichiro Nakanishi, National Astronomical Observatory of Japan – H recombination line observations, a fundamental probe of ionized gas in intrinsically weak lines made accessible by ALMA. – H40alpha at 99GHz. Compare to VLA H53alpha and H92alpha. Telectron is estimated from data. Center has lower Te 6500K, NE region is 9000K. – Metallicity also important (electron donors). – Ionized gas velocity gradient at galaxy center is opposite to that of molecular gas.

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ALMA Science Results

– 17:05 - 17:20 Star formation and turbulence in the Antennae overlap region • Cinthya Herrera, National Astronomical Observatory of Japan – Galaxy interations are key components of galaxy formation and evolution. Most of star formation occurs in very compact (few pc) massive (>10^5 Msun) super star clusters. What triggers their formation? – Cycle 2 data could not see SiO but did get 13CO 2-1. Combine with H2 emission data from VLT. H2 kinematics like CO. – What power H2? Line ratios suggest shocks do the excitation. Where H2/CO is highest is a unique source. An early supercluster? – Also detected unresolved HCN, HCO+ J=4-3 data. FWHM of H2, CO lines is 90 km/s. Looks like H2 cloud is not gravitationally bound. – There are 5 SSCs in the overlap region. – What is the dynamical state of the H2 compact source? We do not see the SiO J=5-4 shock tracer. We expected a source clearly detected.

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ALMA Science Results

– 17:20 - 17:35 Star formation in extreme environments: the case of the prototypical blue compact dwarf II Zw 40 • Amanda Kepley, National Radio Astronomy Observatory – Metallicity and star formation rate surface density critical to understanding; blue compact dwarfs are ideal labs to study these effects. – IIZw40 has low metallicity (0.2 solar) and high star formation rate (0.25 Msun/yr). But low metals makes low dust, gas dissociates – ALMA provides 24pc resolution at high sensitivity. Data at 3mm, 1mm, .8mm, expecting .4mm data. Several giant molecular clouds identified. – Clouds follow size-linewidth relationship generally. CO-H2 conversion factor 5x that in Milky Way. – Molecular gas left in IIZw40 is equal to the mass of its young stars. Can form one more 30Dor-sized cluster.

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ALMA Science Results

– 17:35 - 17:50 WISDOM: mm-wave interferometric survey of dark object masses • Martin Bureau, University of Oxford – Aims: mass assembly history and feedback. Why molecular gas--best tracer of circular velocity in galaxies. Best tracer of dynamical mass. – Get masses of supermassive black holes through CO dynamical measurements. NGC4526 high resolution CO imaging. CARMA data. – Fit to CO rotation curve shows a black hole of 400 million suns. Took 50 hrs of highest resolution A array data. ALMA far faster – No Cyc 2 data yet. Should get three objects soon… Could get a thousand black holes with ALMA.

– 17:50 - 18:05 Investigating the evolution of merging galaxies via cold molecular gas • Junko Ueda, National Astronomical Observatory of Japan – Locally spirals appear to combine, ellipticals result. At z~.65 however, many more peculiar galaxies, which must have evolved to present-day spirals. – Sample of optically selected merger remnants. ALMA observations along with SMA, CARMA. 24 sources modeled. – 54% extended disks. 18

ALMA Science Results

ALMA Postdoctoral Symposium • At NAOJ, Mitaka 13-14 Dec – http://almaintweb.mtk.nao.ac.jp/~cherrera/Home.html

• 26 participants from across ALMA—including Jen, Amanda and Drew • 22 talks on a variety of topics

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ALMA Science Results

Summary? • ALMA’s sensitivity and directivity enable studies of nuclear regions of galaxies – Still difficult to disentangle inflow from outflow; in some cases motions were kinematically complex – One needs a better measure of mass—for most objects only a limit could be established – Excellent prospects for measuring BH masses dynamically

• ALMA’s broad spectral grasp enables parallel excitation analyses among up to ~40 species. • Whither ALMA Development? – – – – 20

Broader spectral coverage—faster data acquisition? Complete the spectral coverage? Longer baselines (e.g. LLAMA project, EHT)? Interpretive and analytical software? ALMA Science Results

ALMA 2030 • Switch to pdfs…

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ALMA Science Results

ALMA OBSERVATIONS OF THE ANTENNAE GALAXIES. I. A NEW WINDOW ON A PROTOTYPICAL MERGER Bradley C. Whitmore et al. 2014 ApJ 795 156

• Filaments identified with beads-on-a-string morphology • Clear evolutionary sequence emerges • Diffuse GMCs beget protoclusters beget embedded clusters beget emerging clusters beget young clusters beget old clusters. • The lifetime of a GMC in a star formation region is of order 10 Myr

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(L) CO J=3-2 knots, (C) 3.7 GHz emission, (R) optical clusters in the Long-Thin filament Green contours (20, 40, 60 K km s−1) show CO emission; ;

and orange provides information about the optical clusters.

ALMA Science Results

Starburst Nuclear Ring Imaged by ALMA in NGC1614 • ALMA resolved CO J=6-5 and 435m continuum emission in this 68Mpc distant LIRG. – Knots in a molecular ring at 100 pc