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Molecular Gas, AGN Feedback, and the Unusual Case of NGC 1266

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Molecular gas, AGN feedback, and the Credit: C. Hull unusual case of NGC 1266 Katey Alatalo March 6, 2012 Collaborators ATLAS3D 3D CO Effort ATLAS Harald Kuntschner Roland Bacon Pierre-Yves Lablanche Katey Alatalo Maxime Bois Richard McDermid Tim Davis Frederic Bounard Raffaella Morganti Lisa Young Michele Cappellari Thorsten Naab Martin Bureau Alison Crocker Tom Oosterloo Leo Blitz Roger Davies Marc Sarzi Tim de Zeeuw Nic Scott Pierre-Alain Duc Paolo Serra NGC1266 Effort Eric Emsellem Remco van den Bosch Carl Heiles Jesus Falcón-Barroso Glenn van de Ven Philip Chang Sadegh Khochfar Gjis Verdoes-Klein Kristen Shapiro Davor Krajnović Anne-Marie Weijmans Laura Lopez ATLAS3D a volume-limited survey of nearby early-type galaxies D < 42 Mpc ATLAS3D ETGs MK < -21.5 9 (Mgal > 6 × 10 M) |δ - 29°| < 35° |b| > 15° 871 possible galaxies morphologically selected (only elliptical, E or lenticular, S0) mass 261 early-type galaxies Cappellari et al. 2011 ATLAS3D : CO Results 22% of ETGs contain molecular gas - no mass or environment preference -strong preference for rotation-dominated - “green valley” objects more likely to contain molecular gas Young et al. 2011 L. Young, Private Communication who said red and dead? 3D NGC4710NGC4710 NGC5379NGC5379 32 galaxies, 30 ATLAS galaxies NGC1266NGC1266 IC0719IC0719 IC 676NGC5866NGC5866 NGC 3626PGC029321PGC029321 NGC 5379 NGC4526NGC4526 NGC4324NGC4324 Complete down to 18.5 Jy km/s IC 719NGC1222NGC1222 NGC 3665NGC0524NGC0524 NGC 5866 (leaving 14 detected faintest galaxies un-imaged) NGC2764NGC2764 NGC3182NGC3182 IC 1024UGC09519UGC09519 NGC 4119NGC6798NGC6798 NGC 6014 NGC7465NGC7465 NGC5173NGC5173 467 hours of CARMA time NGC 1222NGC3665NGC3665 NGC 4292NGC4278NGC4278 NGC 7465 IC0676IC0676 NGC4477NGC4477 5 semesters IC1024IC1024 PGC016060PGC016060 NGC 1266 NGC 4324 PGC029321 NGC4753NGC4753 NGC3489NGC3489 NGC 2697PGC058114PGC058114 NGC 4429NGC4203NGC4203 PGC Pre-ATLAS3D CARMA NGC4459NGC4459 NGC4684NGC4684 NGC3032NGC3032 PGC056772PGC056772 058114 ~20 CO-imaged ETGs NGC3607NGC3607 NGC3156NGC3156 (work of Wrobel & Kenney, L. Young, F. NGC 2764NGC6014NGC6014 NGC 4435NGC2768NGC2768 UGC 05408 Combes, A. Crocker and L. Wei) NGC3626NGC3626 UGC05408UGC05408 NGC 2824NGC4429NGC4429 NGC 4694NGC5273NGC5273 UGC 06176 NGC4694NGC4694 PGC061468PGC061468 Now: NGC 3182NGC4150NGC4150 NGC 4710NGC4111NGC4111 UGC 09519 ~50 (> a factor of 2 increase) NGC4476NGC4476 NGC2685NGC2685 NGC 3607NGC2697NGC2697 NGC 4753NGC3595NGC3595 NGC4435NGC4435 NGC3245NGC3245 3D data cubes (channel maps), integrated NGC 3619NGC4119NGC4119 NGC 5173NGC4283NGC4283 NGC3619NGC3619 NGC4596NGC4596 intensity (mom0) and integrated velocity NGC2824NGC2824 NGC3073NGC3073 (mom1) to be made available publically for UGC06176UGC06176 NGC0509NGC0509 all ATLAS3D galaxies NGC 1266 9 10 M of gas in nuclear region Hosts a massive molecular outflow Local example of AGN feedback? No signs of interaction Alatalo et al. 2011 IRAM 30m CO spectrum Orion outflow Bally & Lada 1983 “typical” E/S0 CO spectrum Δv ≈ 800 km s-1 Velocity (km/s) Combes, Young & Bureau 2007 Nuclear Gas 1266 8 4 × 10 M of gas (H2 + He) is concentrated within central 100 pc 4 -2 Σgas = 2.7×10 M pc -1 -2 expected SFR from K-S: 285 M yr kpc calculated SFR from LFIR and LPAH: Bigiel et al. 2008 -1 -2 ΣSFR(FIR) = 195 M yr kpc -1 -2 ΣSFR(PAH) = 53 M yr kpc NGC 1266 hosts a massive molecular outflow Regular rotation in center 7 Mout(H I + H2) ~ 3 × 10 M dM /dt ~ 13 M yr-1 out assuming an optically thin Rout ~ 450 pc CO-H2 conversion factor tdyn ~ 2.6 Myr tdep ~ 85 Myr Outflow appears to be multi-phase SINGS photometry of Hα show that [S II] from Gemini most of the emission GMOS, which from shock includes the velocity information 1.4 GHz continuum shows both [S II] moment 1 unresolved peak in 900 [S II] moment 0 nucleus and shock “spurs” X-ray data shows bulk of emission is from shock with T ~ 0.5 keV Davis. et al, in prep -900 H I absorption Continuum-subtracted H I profile Comparison of CO(2-1) and H I profiles H I is only found in absorption in NGC 1266, but shares the blueshifted wing emission 20 -2 N(H I)outflow = 9 × 10 cm 6 M(H I)out ≈ 2 × 10 M H I confirms outflow hypothesis (blueshifted material must be in front of continuum source) Driving NGC 1266 Coincident 4-8 keV and 5 GHz continuum = AGN Hard X-rays and radio continuum confirm AGN in system VLBI detection and dust cone -1 Molecular outflow of >13 M yr -1 SFR of 2.2 M yr (from TIR) too low to sustain outflow (Murray et al. 2005) Using the P1.4GHz – Pjet relation from Bîrzan et al. (2008) radio jet contains sufficient mechanical energy (6×1042 ergs s-1) to drive the molecular outflow (1041 ergs s-1) and requires a 2% coupling Other molecular outflows 1000 M82 Arp 220 ) Mrk 231 1 - 100 Arp 220 yr NGC 1266 M82 (M -1 -1 10 dMout/dt ~ 30 M yr dMout/dt ~ 100 M yr /dt M51 discovery: discovery: out Walter et al. 2002 Sakamoto et al. 2009 dM 1 1 10 100 1000 M51 Mrk 231 SFR (M yr-1) NGC 1266 7 Moutflow ~ few × 10 M dM /dt ~ 130 M yr-1 out -1 discovery: dMout,min/dt > 5x SFRmax dMout/dt ~ 4 M yr cannot be driven by star discovery: Feruglio et al. 2010 formation (Murray et al. 2005) Matsushita et al. 2007 no evidence that it has undergone an interaction -1 dMout/dt ~ 13 M yr -1 HCN : >>13 M yr HCN is detected in the outflow 8 Mout ~ few × 10 M -1 dMout/dt ~ 100 M yr wings? NGC 1266 molecular gas HCN detection 8 Mass of the Core ≈ 4 × 10 M Radius of the Core ≈ 60 pc Highly concentrated gas in nucleus 4 -2 Σ sits within the K-S scatter Core Surface Density ≈ 2.7 × 10 M pc SFR ≈ 100× MW 7 8 -1 Outflow mass ≈ few3 × 10× 10 M M Molecular outflow 100 ≥13 M yr -1-1 Outflow mass flux ≈ 10013 M M yr yr CO line wings exceed vesc Outflow energy ≈ 105655 ergs Ionized gas exhibits wings (±700 km s-1) Shocks in X-ray, radio continuum, H I Outflow luminosity ≈ 104241 ergs ss--11 Blueshifted H I absorption Outflow velocity ≈ 400 km s-1 > v esc AGN has energy to drive outflow Outflow dynamical time ≈ 2.6 Myr SFR is unable to sustain outflow Outflow duration <≈ 8510 Myr X-ray and radio confirm presence of AGN Jet power from radio requires 20%2% coupling coupling Unanswered questions Is the outflow in NGC1266 a one-time event? - timescale (few Myr) sufficiently short to explain the discovery of only one 3D event in ATLAS How did the gas get to the center of NGC1266? - accretion event or outside-in? How was the AGN able to accelerate the gas without dissociating it? What are the implications for the high-z universe? The End Tis the last afternoon at 2012 Jets The theorists have argued and laid down their bets The observers agreed It is ALMA we need And contemplate theory their observation upsets courtesy of Doug Johnstone Star formation in the nucleus 4 -2 Σgas = 2.7×10 M pc ΣSFR predicted for H2 using the Kennicutt-Schmidt (K-S) relation: -1 -2 1266 ΣSFR = 274 M yr kpc -1 SFR(TIR) = 2.2 M yr ΣSFR from TIR (Kennicutt 1998): -1 -2 ΣSFR(TIR) = 195 M yr kpc (upper limit: unknown AGN contribution) -1 SFR(24μm) = 1.5 M yr ΣSFR from 24μm (Calzetti et al. 2007): -1 -2 ΣSFR = 133 M yr kpc (unknown AGN contribution) -1 SFR(PAH) = 0.6 M yr ΣSFR from 8μm PAH emission (Falcón- Barroso et al, in prep): -1 -2 Bigiel et al. 2008 ΣSFR(PAH) = 53 M yr kpc (possible PAH destruction due to AGN) CO morphologies NGC 4429 NGC 5379 IC 1024 NGC 6014 Disks PGC 058114 (~40%) Bars, Rings and Spirals (~35%) NGC 3607 NGC 2697 NGC 4324 NGC 4753 NGC 7465 NGC 4694 Molecular gas in ETGs show a large array of structures Disrupted (~25%) Davis et al., in prep; Alatalo et al., in prep Chandra Observations Courtesy of Laura Lopez Full Chandra image 4-8 keV overlaid with 5 GHz Spectrum fit most of the flux with thermal bremsstrahlung (T = 0.5 keV) and minor contribution from a power law component. 4-8 keV photons are cospatial with the 5 GHz peak : AGN The Hubble sequence a morphological classification Late-type galaxies (LTGs) How to create a ETG : mergers “Typical” ETGs A “typical” LTG Early-type galaxies (ETGs) Lenticular / disky S0 disky spiral smooth light profile : lack spiral structure structure blue color ellipsoidal red color Star forming Quiescent Toomre & Toomre 1972 Springel, di Matteo & Hernquist 2005 Elliptical Galaxy color classification How to create a RSG : quench star formation most ETGs are red sequence galaxies red sequence( RSGs) much smaller scatter older stellar populationsconversion to red sequence takes ~1 Gyr after SF blue cloud quenching, large scatter followed by star forming minimal evolution Harker et al. 2006 K. Schawinski Color-Morphology Unification : : galaxies galaxies lacking sitting on the spiral structure red sequence (merged) (quenched) Quiescent “red and dead” ETGs Outliers: Red Spirals Outliers: Blue ETGs 6% are dusty starbursts (Yan et al. 2006) Passive disks see: Masters et al. 2010, Bundy et al. 2010 K. Schawinski “blue” ETGs Masters et al. 2010 Not completely “red and dead” 15% contain H I (Knapp et al. 1985) > 50% have detectable dust (Knapp et al. 1989) 30% have signs of recent star formation in NUV (Kaviraj et al. 2007) Kaviraj et al. 2007 ATLAS3D : Some Results Of the 260 ATLAS3D ETGs: 86% are rotation dominated 68% have ionized gas emission 40%* contain H I 14% are dispersion dominated Private Communication: *(field galaxies, above δ=10°) Krajnović et al. 2011 M. Sarzi Serra et al. 2011 dispersion dominated rotation dominated many CO detections fully virialized within Virgo Young et al.
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    Astronomy & Astrophysics manuscript no. planck c ESO 2018 October 26, 2018 The Herschel Virgo Cluster Survey? XV. Planck submillimetre sources in the Virgo Cluster M. Baes1, D. Herranz2, S. Bianchi3, L. Ciesla4, M. Clemens5, G. De Zotti5, F. Allaert1, R. Auld6, G. J. Bendo7, M. Boquien8, A. Boselli8, D. L. Clements9, L. Cortese10, J. I. Davies6, I. De Looze1, S. di Serego Alighieri3, J. Fritz1, G. Gentile1;11, J. Gonzalez-Nuevo´ 2, T. Hughes1, M. W. L. Smith6, J. Verstappen1, S. Viaene1, and C. Vlahakis12 1 Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281, B-9000 Gent, Belgium 2 Instituto de F´ısica de Cantabria (CSIC-UC), Avda. los Castros s/n, 39005 Santander, Spain 3 INAF - Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125, Florence, Italy 4 University of Crete, Department of Physics, Heraklion 71003, Greece 5 INAF-Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy 6 School of Physics and Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff CF24 3AA, UK 7 UK ALMA Regional Centre Node, Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, United Kingdom 8 Aix Marseille Universite,´ CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France 9 Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, UK 10 Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria, 3122, Australia 11 Department of Physics and Astrophysics, Vrije Universiteit Brussel, Pleinlaan 2, 1050 Brussels, Belgium 12 Joint ALMA Observatory / European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile October 26, 2018 ABSTRACT We cross-correlate the Planck Catalogue of Compact Sources (PCCS) with the fully sampled 84 deg2 Herschel Virgo Cluster Survey (HeViCS) fields.
  • Making a Sky Atlas

    Making a Sky Atlas

    Appendix A Making a Sky Atlas Although a number of very advanced sky atlases are now available in print, none is likely to be ideal for any given task. Published atlases will probably have too few or too many guide stars, too few or too many deep-sky objects plotted in them, wrong- size charts, etc. I found that with MegaStar I could design and make, specifically for my survey, a “just right” personalized atlas. My atlas consists of 108 charts, each about twenty square degrees in size, with guide stars down to magnitude 8.9. I used only the northernmost 78 charts, since I observed the sky only down to –35°. On the charts I plotted only the objects I wanted to observe. In addition I made enlargements of small, overcrowded areas (“quad charts”) as well as separate large-scale charts for the Virgo Galaxy Cluster, the latter with guide stars down to magnitude 11.4. I put the charts in plastic sheet protectors in a three-ring binder, taking them out and plac- ing them on my telescope mount’s clipboard as needed. To find an object I would use the 35 mm finder (except in the Virgo Cluster, where I used the 60 mm as the finder) to point the ensemble of telescopes at the indicated spot among the guide stars. If the object was not seen in the 35 mm, as it usually was not, I would then look in the larger telescopes. If the object was not immediately visible even in the primary telescope – a not uncommon occur- rence due to inexact initial pointing – I would then scan around for it.
  • Emission and Star Formation in Late-Type Galaxies

    Emission and Star Formation in Late-Type Galaxies

    A&A 397, 871–881 (2003) Astronomy DOI: 10.1051/0004-6361:20021572 & c ESO 2003 Astrophysics [C II] emission and star formation in late-type galaxies II. A model? D. Pierini1;2, K. J. Leech3,andH.J.V¨olk4 1 Ritter Astrophysical Research Center, The University of Toledo, Toledo, OH 43606, USA 2 Max-Planck-Institut f¨ur extraterrestrische Physik, Giessenbachstrasse, 85748 Garching, Germany e-mail: [email protected] 3 ISO Data Centre, Astrophysics Division, ESA Space Science Dept., PO Box 50727 Madrid, Spain e-mail: [email protected] 4 Max-Planck-Institut f¨ur Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany e-mail: [email protected] Received 16 August 2001 / Accepted 29 October 2002 Abstract. We study the relationship between gas cooling via the [C II] (λ = 158 µm) line emission and dust cooling via the far- IR continuum emission on the global scale of a galaxy in normal (i.e. non-AGN dominated and non-starburst) late-type systems. It is known that the luminosity ratio of total gas and dust cooling, LCII=LFIR, shows a non-linear behaviour with the equivalent width of the Hα (λ = 6563 Å) line emission, the ratio decreasing in galaxies of lower massive star-formation activity. This result holds despite the fact that known individual Galactic and extragalactic sources of the [C II] line emission show different [C II] line-to-far-IR continuum emission ratios. This non-linear behaviour is reproduced by a simple quantitative theoretical model of gas and dust heating from different stellar populations, assuming that the photoelectric effect on dust, induced by far-UV photons, is the dominant mechanism of gas heating in the general diffuse interstellar medium of the galaxies under investigation.