Presentation is loading. Please wait.

Presentation is loading. Please wait.

1 Center for Astrophysics and Space Astronomy (CASA) Department of Astrophysical and Planetary Sciences (APS) University of Colorado, Boulder The Herschel.

Similar presentations


Presentation on theme: "1 Center for Astrophysics and Space Astronomy (CASA) Department of Astrophysical and Planetary Sciences (APS) University of Colorado, Boulder The Herschel."— Presentation transcript:

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

2 8  m 70  m 350  m Sgr B2 Sgr B1 G0.25 GCB 50 km/s Sgr A 20 km/s

3 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

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

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

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

7 Barred Spiral : NGC1097 HST 1 kpc starburst ring

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

9

10 24  m Bania’s Clump 2 l = 1.3 Sgr B2 / B1 Sgr A Sgr C (Hinz 2008; Yusef-Zadeh 2009)

11 Bania’s Clump 2 l = 1.3 Sgr B2 / B1 Sgr A Sgr C 70  m

12 Bania’s Clump 2 l = 1.3 Sgr B2 / B1 Sgr A Sgr C 160  m

13 Bania’s Clump 2 l = 1.3 Sgr B2 / B1 Sgr A Sgr C 250  m

14 Bania’s Clump 2 l = 1.3 Sgr B2 / B1 Sgr A Sgr C 350  m

15 Bania’s Clump 2 l = 1.3 Sgr B2 / B1 Sgr A Sgr C 500  m

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

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

18 24  m Bania’s Clump 2 l = 1.3 Sgr B2 / B1 Sgr A Sgr C (Hinz 2008; Yusef-Zadeh 2009)

19 Bania’s Clump 2 l = 1.3 Sgr B2 / B1 Sgr A Sgr C 70  m

20

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

22 Central Molecular Zone

23 20 cm, 70  m, 350  m

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

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

26

27 24  m 350  m 2/3 gas, Pos. longitudes 2/3 24  m Neg. longitudes Sgr A* Inert, stable CMZ Starburst region 1 o => R ~ 150 pc, t orbit ~ 8 Myr Sgr B2

28 Central Molecular Zone (CMZ) - x10 - x100 denser, more turbulent than disk GMCs Traced by HCN, HNCO, CS, SiO, NH 3, etc.  V > 20 km/s - Asymmetry: Gas & cold dust: 2/3 at POSITIVE longitude, velocity 24  m sources: 2/3 at NEGATIVE longitude Note: t orbit ~ 6 Myr r 100 pc V 100 km/s -1 (+ 3 to 30 Myr)

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

30 Sgr A (CNR) N(H 2 ) from dust (Rome algorithm)

31 T dust cold ~ 14 K warm ~ 50 K (Rome algorithm) Sgr A (CNR)

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

33 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?

34

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

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

37 8  m 70  m 350  m Sgr A (CNR )

38 Galactic Center: 20 cm Sgr A (CNR )

39 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 ?

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

41 Sgr B2 Continuum CO SED (Etxaluze )

42 3.6, 4.5, 8  m 280 GHz continuum 2.12  m H 2 Sgr C (G ) Kendrew et al. poster

43 Bania’s Clump 2 l = 3.2 o 10 6 M o Most CMZ molecular gas at positive Longitudes, & positive Velocities

44 Dense Gas with little / no star formation Bania’s Clump 2 (l = 3.2 o ) & l = 1.3 o o - 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 ?

45 Bania’s Clump 2 24 um, 70 um, 350 um

46 G (the “Brick” or “Lima Bean”) 10 5 M o 3 pc, dense cloud in CMZ VERY LITTLE STAR FORMATION ! (the most extreme IRDC in the Galaxy?) (Longmore et al. 2012) - ALMA Cycle 0 data (Rathborne et al. 2013)  m (Spitzer) 70  m (Hi-GAL) 450  m (SCUBA)

47

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

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

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

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

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

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

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

55

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

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

58 CNR HIFI (Herschel) (Sonnentrucker ) 50 km/s cloud 20 km/s cloud CNR HIFI (Herschel)/GREAT (SOFIA) (Requena-Torres ) Hot (400 K) CO in 3 pc ring HF & para H 2 O in CMZ

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

60 Summary ~ 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 = 1.3 o, Bania’s Clump 2 (l = 3.2 o ), 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, … M o /yr ? Variable?

61


Download ppt "1 Center for Astrophysics and Space Astronomy (CASA) Department of Astrophysical and Planetary Sciences (APS) University of Colorado, Boulder The Herschel."

Similar presentations


Ads by Google