Hi-GAL PI: Sergio Molinari (Rome) + Hi-GAL team … (~150 researchers)

Slides:

Advertisements

Similar presentations

From GMC-SNR interaction to gas-rich galaxy-galaxy merging Yu GAO Purple Mountain Observatory, Nanjing, China Chinese Academy of Sciences.

Advertisements

Toyoaki Suzuki (ISAS/JAXA) Hidehiro Kaneda (Nagoya Univ.) Takashi Onaka (Tokyo Univ.)

Fluorescent Processes Research School of Astronomy & Astrophysics Fluorescent Processes Feeding The Beast: Infall, Mergers or Starbursts? Mike Dopita (ANU)

Our Galaxy `. Interstellar dust obscures our view at visible wavelengths along lines of sight that lie in the plane of the galactic disk.

John Bally Center for Astrophysics and Space Astronomy Department of Astrophysical and Planetary Sciences University of Colorado, Boulder Star Formation.

Low Energy measurements of Cosmic Rays suggested by the HE group 1 1Tracing the distribution of matter in order to understand HE data Measurements of NH.

The Galactic Center: Molecular Line Mapping with Broadband Spectrometers Jürgen Ott ESO 3D Meeting 11 June 2008 The Galactic Center: Molecular Line Mapping.

A MOPRA CS(1-0) demonstration survey of the Galactic plane G. Fuller, N. Peretto, L. Quinn (University of Manchester UK), J. Green (ATNF ) All dust continuum.

Loránt Sjouwerman, Ylva Pihlström & Vincent Fish.

PRISMAS PRISMAS PRobing InterStellar Molecules with Absorption line Studies M. Gerin, M. Ruaud, M. de Luca J. Cernicharo, E. Falgarone, B. Godard, J. Goicoechea,

Gas and Star Formation in the Circinus Galaxy Bi-Qing For ( 傅碧晴 ) SIEF John Stocker Fellow ICRAR / University of Western Australia Baerbel Koribalski (CSIRO.

Multi-band Infrared Mapping of the Galactic Nuclear Region Q. D. Wang (PI), H. Dong, D. Calzetti (Umass), Cotera (SETI), S. Stolovy, M. Muno, J. Mauerhan,

Portrait of a Forming Massive Protocluster: NGC6334 I(N) Todd Hunter (NRAO/North American ALMA Science Center) Collaborators: Crystal Brogan (NRAO) Ken.

EGOs: Massive YSOs in IRDCs Ed Churchwell & Claudia Cyganowski with co-workers: Crystal Brogan, Todd Hunter, Barb Whitney Qizhou Zhang Dense Cores in Dark.

CO J =1-0 + J =3-2 map (Oka+ 1999, 2007) Galactic Center Kunihiko Tanaka (1), Tomoharu Oka (1), Shinji Matsumura (1), Kazuhisa Kamegai (2), Makoto Nagai.

Submillimeter Astronomy in the era of the SMA, 2005, Cambridge, MA Observations of Extragalactic Star Formation in [CI] (370  m) and CO J=7-6 T. Nikola.

Hot and Diffuse Gas near the Galactic Center Probed by Metastable H 3 + Thomas R. Geballe Gemini Observatory Miwa Goto Max Planck Institute for Astronomy.

STAR FORMATION STUDIES with the CORNELL-CALTECH ATACAMA TELESCOPE Star Formation/ISM Working Group Paul F. Goldsmith (Cornell) & Neal. J. Evans II (Univ.

H3+H3+. Search for hot and bright stars for H 3 + spectroscopy Near the Galactic center Takeshi Oka Department of Astronomy and Astrophysics and Department.

A Submillimeter study of the Magellanic Clouds Tetsuhiro Minamidani (Nagoya University) & NANTEN team ASTE team Mopra – ATNF team.

The Galactic center region Concentrated stars and interstellar matter High energy density (gravity, MHD, kinetic) Strong magnetic field :B ~ mG High external.

A Herschel Galactic Plane Survey of [NII] Emission: Preliminary Results Paul F. Goldsmith Umut Yildiz William D. Langer Jorge L. Pineda Jet Propulsion.

The Milky Way and Other Galaxies Science A-36 12/4/2007.

Star Formation Research Now & With ALMA Debra Shepherd National Radio Astronomy Observatory ALMA Specifications: Today’s (sub)millimeter interferometers.

TURBULENCE AND HEATING OF MOLECULAR CLOUDS IN THE GALACTIC CENTER: Natalie Butterfield (UIowa) Cornelia Lang (UIowa) Betsy Mills (NRAO) Dominic Ludovici.

MALT 90 Millimetre Astronomy Legacy Team 90 GHz survey

Der Paul van der Werf Leiden Observatory H 2 emission as a diagnostic of physical processes in star forming galaxies Paris October 1, 1999.

Molecular absorption in Cen A on VLBI scales Huib Jan van Langevelde, JIVE Ylva Pihlström, NRAO Tony Beasley, CARMA.

Initial Conditions for Star Formation Neal J. Evans II.

HOPS – The H 2 O southern Galactic Plane Survey Image Courtesy: Cormac Purcell.

The Galactic Center at Low Radio Frequencies Namir Kassim (NRL) Crystal Brogan (IfA) J. Lazio (NRL), Ted LaRosa (Kennesaw State), M. Nord (NRL/UNM), W.

Star Formation in our Galaxy Dr Andrew Walsh (James Cook University, Australia) Lecture 1 – Introduction to Star Formation Throughout the Galaxy Lecture.

Gas Dynamics, AGN, Star Formation and ISM in Nearby Galaxies Eva Schinnerer (MPIA) S. Haan, F. Combes, S. Garcia-Burillo, C.G. Mundell, T. Böker, D.S.

The Incredible 6.7 GHz Methanol Masers: A key to understanding high-mass star formation. Jimi Green (for Gary Fuller) CSIRO Astronomy & Space Science,

Direct Physical Diagnostics of Triggered Star Formation Rachel Friesen NRAO Postdoctoral Fellow North American ALMA Science Center C. Brogan, R. Indebetouw,

Interstellar Matter and Star Formation in the Magellanic Clouds François Boulanger (IAS) Collaborators: Caroline Bot (SSC), Emilie Habart (IAS), Monica.

Quiz 3 Briefly explain how a low-mass star becomes hot enough to settle on the main-sequence. Describe what is solar weather and list two ways in which.

Molecular Gas (Excitation) at High Redshift Fabian Walter Max Planck Institute for Astronomy Heidelberg Fabian Walter Max Planck Institute for Astronomy.

ASTR112 The Galaxy Lecture 7 Prof. John Hearnshaw 11. The galactic nucleus and central bulge 11.1 Infrared observations (cont.) 11.2 Radio observations.

Warm Molecular Gas in Galaxies Rui-Qing Mao ( 毛瑞青 ) (Purple Mountain Observatory, Nanjing) C. Henkel (MPIfR) R. Mauersberger (IRAM) Dinh-Van-Trung (ASIAA)

An Evolutionary Model of Submillimeter Galaxies Sukanya Chakrabarti NSF Fellow CFA.

H 3 + Toward and Within the Galactic Center Tom Geballe, Gemini Observatory With thanks to Takeshi Oka, Ben McCall, Miwa Goto, Tomonori Usuda.

EXPANDING DIFFUSE MOLECULAR GAS IN THE CENTRAL MOLECULAR ZONE OF THE GALACTIC CENTER PROBED BY H th International Symposium on Molecular Spectroscopy.

Philamentary Structure and Velocity Gradients in the Orion A Cloud

Jet Propulsion Laboratory

ALMA: Imaging the cold Universe Great observatories May 2006 C. Carilli (NRAO) National Research Council Canada.

Early O-Type Stars in the W51-IRS2 Cluster A template to study the most massive (proto)stars Luis Zapata Max Planck Institut für Radioastronomie, GERMANY.

Cornelia C. Lang University of Iowa collaborators:

Universe Tenth Edition

HST HII regions & optical light Eva Schinnerer Max Planck Institute for Astronomy molecular gas (PAWS) 1 kpc Star Formation and ISM in Nearby Galaxies:

Our Galaxy Chapter Twenty-Five. Guiding Questions 1.What is our Galaxy? How do astronomers know where we are located within it? 2.What is the shape and.

Low-luminosity Extragalactic H 2 O Masers Yoshiaki Hagiwara ASTRON.

First high-resolution 3D inversion of the dust emission in Galactic ISM with Spitzer/Herschel. The case region [l,b]=[30,0] A. Traficante, R. Paladini,

Simulations for the nearby Seyfert 2 galaxy NGC 4945 Lien-Hsuan Lin 1,2, Chi Yuan 2, C.C. D. Yen 3, and S. Muller 2 1 Department of Physics, National Taiwan.

XGAL 2016, Charlottesville, April 5 th 2016 Sergio Martín Ruiz Joint ALMA Office The unbearable opaqueness of obscured nuclei.

High Redshift Galaxies/Galaxy Surveys ALMA Community Day April 18, 2011 Neal A. Miller University of Maryland.

The Physics of Galaxy Formation. Daniel Ceverino (NMSU/Hebrew U.) Anatoly Klypin, Chris Churchill, Glenn Kacprzak (NMSU) Socorro, 2008.

John Bally Center for Astrophysics and Space Astronomy Department of Astrophysical and Planetary Sciences University of Colorado, Boulder Recent Developments.

Bolocam Galactic Plane Survey Herschel Hi-GAL Plane Survey

Filamentary Structures Traced by IRDCs

The MALT90 survey of massive star forming regions

Excitation of H2 in NGC 253 Marissa Rosenberg

Molecular Gas Distribution of our Galaxy: NANTEN Galactic Plane Survey

LARGE PICTURE OF THE GALACTIC CENTER STUDIED BY H3+:

Morphology of the Galactic center from the H3+ spectrum:

Chemical evolution of N2H+ in massive star-forming regions

Millimeter Megamasers and AGN Feedback

Cornelia C. Lang University of Iowa collaborators:

Presentation transcript:

Hi-GAL PI: Sergio Molinari (Rome) + Hi-GAL team … (~150 researchers) The Herschel View of the Galactic Center John Bally1 Hi-GAL PI: Sergio Molinari (Rome) + Hi-GAL team … (~150 researchers) 1Center for Astrophysics and Space Astronomy (CASA) Department of Astrophysical and Planetary Sciences (APS) University of Colorado, Boulder

Sgr B2 Sgr B1 G0.25 GCB 50 km/s Sgr A 20 km/s 8 m 70 m 350 m

Outline Herschel Hi-GAL: 70, 160, 250, 350, 500 m The Central Molecular Zone: Context Dust Cold dust, (warm gas); Column density Star Formation Distribution, Asymmetries, Rate Galactic Center Bubble: Relation to: Sofue-Handa Lobe, Fermi/LAT, … Nature of 70 m sources Star Formation vs. SMBH activity: Feeding vs. Shielding

Herschel Space Observatory: (May 2009 - April 2013) D = 3.5 meter @ L2 PACS: 70, 100, 160 m SPIRE: 250, 350, 500 m HIFI: THz heterodyne Herschel Galactic Plane Survey (Hi-GAL)

Herschel Galactic Plane Survey (Hi-GAL) PI: Sergio Molinari (Rome) + 150 co-Is ~900 hrs Galactic Plane [360o X 2o] 720 square degree survey  = 70, 160, 250, 350, 500 m  = 6 , 11, 15 , 22 , 35 arcsec resolution Hi-GAL - inner Galaxy 120o year 1 Hi-GAL360 - outer Galaxy 120o year 2 2-GAL - 60o segments at l = 90o, 270o year 3 Images & Catalogs in preparation (release in late 2013) ~ 500,000 band-merged compact sources (YSOs, compact HII regions, post-MS stars, PNe, …)

(tri-axial) potential: x1 vs. x2 The CMZ: Orbits in a Bar (tri-axial) potential: x1 vs. x2 Inner Lindblad Resonance (ILR) R ~ 450 pc ? Epicyclic frequency Bar rotation frequency ~ 2:1 1.3 kpc

Barred Spiral : NGC1097 HST 1 kpc starburst ring

Orbits: x1 - elongated along bar x2 - elongated orthogonal to bar V l Bally 2010 cartoon Rodriguez-Fernandez 2006, 2008; model Molinari et al. (2011) ring

24 m (Hinz 2008; Yusef-Zadeh 2009) Bania’s Clump 2 l = 1.3 Sgr B2 / B1 Sgr A Sgr C 24 m (Hinz 2008; Yusef-Zadeh 2009)

Bania’s Clump 2 l = 1.3 Sgr B2 / B1 Sgr A Sgr C

Bania’s Clump 2 l = 1.3 Sgr B2 / B1 Sgr A Sgr C

Bania’s Clump 2 l = 1.3 Sgr B2 / B1 Sgr A Sgr C

Bania’s Clump 2 l = 1.3 Sgr B2 / B1 Sgr A Sgr C

Bania’s Clump 2 l = 1.3 Sgr B2 / B1 Sgr A Sgr C

(Bolocam Galactic Plane Survey Ginsburg et al. 2012) Bania’s Clump 2 l = 1.3 Sgr B2 / B1 Sgr A Sgr C 1100 m (Bolocam Galactic Plane Survey Ginsburg et al. 2012)

Bania’s Clump 2 l = 1.3 Sgr B2 / B1 Sgr A Sgr C 20 cm (Yusef-Zadeh 2009)

24 m (Hinz 2008; Yusef-Zadeh 2009) Bania’s Clump 2 l = 1.3 Sgr B2 / B1 Sgr A Sgr C 24 m (Hinz 2008; Yusef-Zadeh 2009)

Bania’s Clump 2 l = 1.3 Sgr B2 / B1 Sgr A Sgr C

Central Molecular Zone 24 m, 70 m, 350 m

Central Molecular Zone 24 m, 70 m, 350 m

Central Molecular Zone 20 cm, 70 m, 350 m

Central Molecular Zone 20 cm, 70 m, 350 m

Central Molecular Zone 20 cm, 70 m, 350 m

2/3 gas, dust: @ Pos. longitudes 2/3 24 m sources: @ Neg. longitudes 24 m 350 m 2/3 gas, dust: @ Pos. longitudes 2/3 24 m sources: @ Neg. longitudes 1o => R ~ 150 pc, torbit ~ 8 Myr Sgr B2 Sgr A* Inert, stable CMZ Starburst region

Central Molecular Zone (CMZ) - x10 - x100 denser, more turbulent than disk GMCs Traced by HCN, HNCO, CS, SiO, NH3, etc. V > 20 km/s Asymmetry: Gas & cold dust: 2/3 at POSITIVE longitude, velocity 24 m sources: 2/3 at NEGATIVE longitude Note: torbit ~ 6 Myr r100 pc V100 km/s-1 (+ 3 to 30 Myr)

Dust T, N(H2) Battersby (2011, A&A, 535, 128) algorithm cold ~ 14 K warm ~ 50 K N(H2) 2 x 1021 to 2 x 1024 cm-2

N(H2) from dust (Rome algorithm) Sgr A (CNR)

Tdust cold ~ 14 K warm ~ 50 K (Rome algorithm) Sgr A (CNR)

The Molinari et al. (2011) ~100 pc ring Sgr A (CNR)

The Molinari et al. (2011) R ~100 pc ring Region of Starburst activity in CMZ But … Sgr B2 Proper Motion ~ 80 km/s => R ~ 150 to 200 pc?

Galactic Center: 8 m Sgr B2 Sgr A (CNR)

Galactic Center Bubble: 24 m Sgr A (CNR)

Sgr A (CNR) 8 m 70 m 350 m

Galactic Center: 20 cm Sgr A (CNR)

Galactic Center Bubble - Brightest super-bubble in Galaxy at 24 m - D ~ 30 pc - Arches, Pistol clusters, Sgr A East SNR A nested set of Bubbles? Sgr A East: 1 pc GCB: 30 pc Sofue-Handa (84) lobe: 150 pc Fermi-LAT bubble: 5,000 pc A weak `nuclear super-wind’ ? Star-formation -or- SMBH ?

Galactic Center Bubble => Sofue-Handa Lobe => Fermi-LAT Bubble ? Finkbeiner et al. (2010) Caution: Sco-Cen superbubble 150 pc from Sun Sofue- Handa Lobe 3.5 cm (GBT) 2 deg. Law et al. (2009, 2010)

Sgr B2 Continuum CO SED (Etxaluze+ 2013)

Sgr C (G359.44-.10) Kendrew et al. poster 3.6, 4.5, 8 m 280 GHz continuum 2.12 m H2

Bania’s Clump 2 l = 3.2o 106 Mo Most CMZ molecular gas at positive Longitudes, & positive Velocities

Dense Gas with little / no star formation Bania’s Clump 2 (l = 3.2o) & l = 1.3o - 1.5o - Little 8, 24, 70 m emission - Little or no star-formation - Strong thermal SiO => shocks? Location: At end of innermost x1 orbit ? Along length of x1 orbit ? Where x1 and x2 intersect ?

Bania’s Clump 2 24 um, 70 um, 350 um

G0.253+0.016 (the “Brick” or “Lima Bean”) 105 Mo 3 pc, dense cloud in CMZ VERY LITTLE STAR FORMATION ! (the most extreme IRDC in the Galaxy?) 3.6 - 8.0 m (Spitzer) 70 m (Hi-GAL) 450 m (SCUBA) (Longmore et al. 2012) - ALMA Cycle 0 data (Rathborne et al. 2013)

HCO+ J = 1-0 21 km/s 18 km/s 14 km/s ALMA Cycle 0 data Rathborne et al. 2013 Bally et al. 2013

HCO+ J = 1-0 28 km/s 24 km/s 21 km/s ALMA Cycle 0 data Rathborne et al. 2013 Bally et al. 2013

HCO+ J = 1-0 34 km/s 31 km/s 28 km/s ALMA Cycle 0 data Rathborne et al. 2013 Bally et al. 2013

HCO+ J = 1-0 41 km/s 38 km/s 34 km/s ALMA Cycle 0 data Rathborne et al. 2013 Bally et al. 2013

HCO+ J = 1-0 48 km/s 44 km/s 41 km/s ALMA Cycle 0 data Rathborne et al. 2013 Bally et al. 2013

HCO+ J = 1-0 55 km/s 51 km/s 48 km/s ALMA Cycle 0 data Rathborne et al. 2013 Bally et al. 2013

HCO+ J = 1-0 62 km/s 58 km/s 55 km/s ALMA Cycle 0 data Rathborne et al. 2013 Bally et al. 2013

Sgr A & Circum Nuclear Ring (CNR): 70 um, 160 um, 350 um (SHARC/CSO) Black Hole HCN (1-0) + P 50 km/s cloud 20 km/s cloud Feeding star formation in the CNR? Sgr A cluster L-band: (Viehmann 06)

Hot (400 K), dense molecular gas CO in 3 pc ring Sgr A PACS/SPIRE spectrum (Goicoechea+ 2013)

HF & para H2O in CMZ Hot (400 K) CO in 3 pc ring CNR HIFI (Herschel) (Sonnentrucker+ 2013) CNR HIFI (Herschel)/GREAT (SOFIA) (Requena-Torres+ 2013) 50 km/s cloud 20 km/s cloud

Future - ALMA small-scale line / continuum / polarization - SOFIA HAWC++ MIR continuum / polarization / narrow-band GREAT CII, NII, OI, OIII, etc. FORCAST 11 - 37 um continuum - JVLA NH3, SiO, CS, H2CO / high-f continuum / RRLs - CCAT large-scale CI, CO 4-3 / continuum - JWST small-scale 2 - 28 um

Summary ~ 90 - 150 pc ring of cold dust and gas Contains Sgr B2, Sgr B1, Brick, Sgr C Most extreme star formation at r < 100 pc Large V features: l = 1.3o, Bania’s Clump 2 (l = 3.2o), No (or little) star formation: Galactic Center Bubble: 70 m: YSOs or externally heated? Multiple SN, massive star winds, ionization Feeds Sofue-Handa Lobe (~1 deg.) ? Fermi-LAT Bubble (> 20 deg.) ? Star Formation in the CMZ: “Mini-starbursts” in Sgr B2 Asymmetry: Gas-dust at Positive longitude/velocity 24 m sources at Negative longitude 24 m sources: MYSOs, MS-stars - or - externally illuminated OH/IR, RSG, PNe, … <SFR> 0.007 - 0.1 Mo/yr ? Variable?