The Milky Way Laboratory. Cara Battersby Harvard-Smithsonian Center for Astrophysics

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1 The Milky Way Laboratory Cara Battersby Harvard-Smithsonian Center for Astrophysics

2 The Milky Way Laboratory Figure Credit: NASA / JPL-Caltech / R. Hurt (SSC-Caltech)

3 The Milky Way Laboratory 1. What is the large-scale structure of our Galaxy? 2. How do the most massive stars form in our Galaxy? 3. How do they form in the distant Universe?

4 The Milky Way Laboratory 1. What is the large-scale structure of our Galaxy? 2. How do the most massive stars form in our Galaxy? 3. How do they form in the distant Universe?

5 The Milky Way Laboratory Stop 1: The Skeleton of the Milky Way Nessie Figure Credit: NASA / JPL-Caltech / R. Hurt (SSC-Caltech)

6 The Milky Way Laboratory 1. What is the large-scale structure of our Galaxy? 2. How do the most massive stars form in our Galaxy? 3. How do they form in the distant Universe?

7 The Milky Way Laboratory Stop 2: Massive star and cluster formation Figure Credit: NASA / JPL-Caltech / R. Hurt (SSC-Caltech)

8 The Milky Way Laboratory 1. What is the large-scale structure of our Galaxy? 2. How do the most massive stars form in our Galaxy? 3. How do they form in the distant Universe?

9 The Milky Way Laboratory Stop 3: Extreme SF in our Galactic Center Figure Credit: NASA / JPL-Caltech / R. Hurt (SSC-Caltech)

10 The Milky Way Laboratory Stop 1: The Skeleton of the Milky Way

11 The Skeleton of the Milky Way

12 M51: the Whirlpool Galaxy From the Hubble Space Telescope. NASA / JPL-Caltech / R. Kennicutt (U. Arizona)

13 IC 342 Infrared image Spitzer's infrared array camera (IRAC) are shown in blue (3.6 and 4.5 microns) and green (5.8 and 8.0 microns), while the multiband imaging photometer (MIPS) observation is red (24 microns).

15 Nessie Bone of the Milky Way? 10 pc Goodman et al Red: 24 μm, Green: 8 μm, Blue: 4.5 μm, MIPSGAL (Carey et al. 2009) and GLIMPSE (Benjamin et al. 2003)

16 Nessie Bone of the Milky Way? Goodman et al Red: 24 μm, Green: 8 μm, Blue: 4.5 μm, MIPSGAL (Carey et al. 2009) and GLIMPSE (Benjamin et al. 2003)

17 Nessie Bone of the Milky Way? Goodman et al Red: 24 μm, Green: 8 μm, Blue: 4.5 μm, MIPSGAL (Carey et al. 2009) and GLIMPSE (Benjamin et al. 2003)

18 Nessie Bone of the Milky Way? Goodman et al Dame & Thaddeus 2011

19 Nessie traces out the Scutum- Centaurus Arm. Are there others?

20 Nessie traces out the Scutum- Centaurus Arm. Are there others? Yes!

21 Search for more Bones of the Milky Way Catherine Zucker 2014 SAO REU from Virginia Just started Harvard PhD program! Zucker, Battersby, & Goodman 2015 Red: 24 μm, Green: 8 μm, Blue: 4.5 μm, MIPSGAL (Carey et al. 2009) and GLIMPSE (Benjamin et al. 2003)

22 Search for more Bones of the Milky Way Mid-infrared extinction feature Roughly parallel to the Galactic plane Within 20 pc of the physical Galactic mid-plane Within 10 km/s of the global-log spiral fit to any MW arm Projected aspect ratio greater than or equal to 50:1 Zucker, Battersby, & Goodman 2015 Red: 24 μm, Green: 8 μm, Blue: 4.5 μm, MIPSGAL (Carey et al. 2009) and GLIMPSE (Benjamin et al. 2003)

23 Search for more Bones of the Milky Way BC1 6/10 candidates are excellent tracers of spiral arm in 3-D (position-position-velocity space) We are now working to assemble a full Skeleton Zucker, Battersby, & Goodman 2015

24 Bones of the Milky Way BC1 Working to characterize their physical properties and kinematics with Harvard undergraduate, Amy Cohn Zucker, Battersby, & Goodman 2015

25 Next Steps: The Skeleton of the Milky Way

26 Next Steps: The Skeleton of the Milky Way Identify more Bones of the Milky Way. Combine with other tracers (e.g. CO, HI, dense gas) to develop a model of Galactic structure

27 Next Steps: The Skeleton of the Milky Way Identify more Bones of the Milky Way. Combine with other tracers (e.g. CO, HI, dense gas) to develop a model of Galactic structure Measure physical properties and kinematics of Bones compare directly with simulations. Develop improved Galactic-scale simulations

28 Next Steps: The Skeleton of the Milky Way Identify more Bones of the Milky Way. Combine with other tracers (e.g. CO, HI, dense gas) to develop a model of Galactic structure BC1 Preliminary C 18 O contours on 8μm image Measure physical properties and kinematics of Bones compare directly with simulations. Develop improved Galactic-scale simulations 60 hour IRAM Project (PI: Battersby) to map our best Northern Bone candidate

29 Next Steps: The Skeleton of the Milky Way Identify more Bones of the Milky Way. Combine with other tracers (e.g. CO, HI, dense gas) to develop a model of Galactic structure Smith et al Measure physical properties and kinematics of Bones compare directly with simulations. Develop improved Galactic-scale simulations Butler, Tan, & Van Loo 2015

30 Next Steps: The Skeleton of the Milky Way Identify more Bones of the Milky Way. Combine with other tracers (e.g. CO, HI, dense gas) to develop a model of Galactic structure Measure physical properties and kinematics of Bones compare directly with simulations. Develop improved Galactic-scale simulations Detect Bones in nearby face-on spiral galaxies to understand their role in Galactic structure

structure Measure physical properties and

31 Next Steps: The Skeleton of the Milky Way Identify more Bones of the Milky Way. Combine with other tracers (e.g. CO, HI, dense gas) to develop a model of Galactic structure Measure physical properties and kinematics of Bones compare directly with simulations. Develop improved Galactic-scale simulations Detect Bones in nearby face-on spiral galaxies to understand their role in Galactic structure

CO, HI, dense gas) to develop a model of Galactic structure Measure physical properties and

32 Next Steps: The Skeleton of the Milky Way Identify more Bones of the Milky Way. Combine with other tracers (e.g. CO, HI, dense gas) to develop a model of Galactic structure Measure physical properties and kinematics of Bones compare directly with simulations. Develop improved Galactic-scale simulations Detect Bones in nearby face-on spiral galaxies to understand their role in Galactic structure

33 The Milky Way Laboratory 1. What is the large-scale structure of our Galaxy? 2. How do the most massive stars form in our Galaxy? 3. How do they form in the distant Universe?

34 The Milky Way Laboratory Stop 2: Massive star and cluster formation Figure Credit: NASA / JPL-Caltech / R. Hurt (SSC-Caltech)

35 Evolution Starless proto-cluster Star-forming proto-cluster Star-forming proto-cluster Embedded cluster Battersby et al. 2010; 2011

36 Search for Starless Proto-Clusters

37 Search for Starless Proto-Clusters Embedded cluster

38 Search for Starless Proto-Clusters First ever complete search for massive, compact starless protoclusters (BGPS: Ginsburg, Battersby, et al. 2012) Massive, Tightly Bound: 3 x10 4 M (1 x10 4 M ) r < 2.5 pc Starless proto-cluster Embedded cluster

39 Search for Starless Proto-Clusters First ever complete search for massive, compact starless protoclusters (BGPS: Ginsburg, Battersby, et al. 2012) Massive, Tightly Bound: 3 x10 4 M (1 x10 4 M ) r < 2.5 pc yields 3 (18), none of which are starless G (Longmore et al. 2012) Starless proto-cluster Embedded cluster

40 Search for Starless Proto-Clusters First ever complete search for massive, compact starless protoclusters (BGPS: Ginsburg, Battersby, et al. 2012) Massive, Tightly Bound: 3 x10 4 M (1 x10 4 M ) r < 2.5 pc yields 3 (18), none of which are starless G (Longmore et al. 2012) Starless proto-cluster Embedded cluster

41 Search for Starless Proto-Clusters Starless clumps are *less massive* overall corresponds to mass accretion rate of ~1000 M / Myr Svoboda, Shirley, Battersby, et al G (Longmore et al. 2012) Starless proto-cluster Embedded cluster

42 Search for Starless Proto-Clusters Starless clumps are *less massive* overall corresponds to mass accretion rate of ~1000 M / Myr Svoboda, Shirley, Battersby, et al Follow-up SMA and ALMA surveys toward most massive starless clumps initial structure before disruption by stellar feedback G (Longmore et al. 2012) Starless proto-cluster Embedded cluster

43 5 pc 70 μm, 24 μm, 8 μm From Battersby et al. 2014b; Hi-GAL: Molinari et al. (2011), MIPSGAL: Carey et al. (2009), GLIMPSE: Benjamin et al. (2003),

44 look for evidence of infall in line asymmetries 70 μm, 24 μm, 8 μm, Herschel N(H 2 ) contours G , Battersby+ in prep

45 Intensity Infall Signature Diffuse Dense Emits Diffuse Absorbs Redshifted Blueshifted Pink optically thin sees the entire cloud Cyan optically thick only sees envelope Velocity

46 HCO + (1-0) and H 13 CO + (1-0) on the ARO 12m 70 FWHM 1.8 pc at 5.5 kpc G , Battersby, Myers, Keto, et al. in prep

47 HCO + (1-0) and H 13 CO + (1-0) on the ARO 12m Clear evidence of infall 70 FWHM 1.8 pc at 5.5 kpc G , Battersby, Myers, Keto, et al. in prep

48 Perform modified blackbody fitting of Herschel data to derive N(H 2 ) and dust temperature. 70 μm, 24 μm, 8 μm, Herschel N(H 2 ) contours G , Battersby, Myers, Keto, et al. in prep

49 Add the density and temperature profiles v in Density Profile Temp Profile 70 μm, 24 μm, 8 μm, Herschel N(H 2 ) contours

50 N(H 2 ) [x cm -2 ] cm -2 ] Dust Temperature [K] N(H 2 ) [x Radius 2 [pc] Radius Radius 1 [pc] Use our knowledge of the physical structure to inform the radiative transfer model (MOLLIE) Plummer profile, p = 2, rflat = 0.5 pc MOLLIE fit Flat temperature profile, T = 16 K 3 Battersby, Myers, Keto, et al. in prep

51 Calculate infall rates 1 pc Density Profile Temp Profile V in = 2km/s Density from Plummer fit Surface area of cylinder HCO + line profile fit

52 3 different densities V in = 2km/s 1 pc Densit y Profile Temp Profile Density from Plummer fit Surface area of cylinder HCO + line profile fit

53 Mass/length [M / pc] Infall Rates [M per pc per Myr] High density Distance Along Filament [pc] Average density Low density Battersby et al., in prep. See also Peretto et al. (2013), SDC335 Mass infall rate of 700 M / Myr.

54 Mass/length [M / pc] 5000 Infall Rates Region can double its mass in a Myr! [M per pc per Myr] High density Distance Along Filament [pc] Average density Low density Battersby et al., in prep. See also Peretto et al. (2013), SDC335 Mass infall rate of 700 M / Myr.

55 Evolution Starless proto-cluster Star-forming proto-cluster Star-forming proto-cluster Embedded cluster Battersby et al. 2010; 2011

56 (e.g. Battersby et al. in prep., Longmore et al. (2011); Schneider et al. 2010; Barnes et al. 2010; Galván-Madrid et al. 2010; Liu et al. 2012) Quiescent Starless -- mid-ir proto-cluster dark Star-forming proto-cluster Star-forming proto-cluster Embedded cluster

57 Next Steps: Massive Star and Cluster Formation

58 Next Steps: Massive Star and Cluster Formation Add more species and improve radiative transfer modeling (JCMT, PI: Kirk).

59 Next Steps: Massive Star and Cluster Formation Add more species and improve radiative transfer modeling (JCMT, PI: Kirk). Measure infall rates toward many more regions. Does it correlate with mass or evolutionary stage? What determines the final mass of a cluster?

60 Next Steps: Massive Star and Cluster Formation Add more species and improve radiative transfer modeling (JCMT, PI: Battersby). Measure infall rates toward many more regions. Does it correlate with mass or evolutionary stage? What determines the final mass of a cluster?

61 Next Steps: Massive Star and Cluster Formation Add more species and improve radiative transfer modeling (JCMT, PI: Kirk). Measure infall rates toward many more regions. Does it correlate with mass or evolutionary stage? What determines the final mass of a cluster?

62 The Milky Way Laboratory 1. What is the large-scale structure of our Galaxy? 2. How do the most massive stars form in our Galaxy? 3. How do they form in the distant Universe?

63 The Milky Way Laboratory Stop 3: Extreme SF in our Galactic Center Figure Credit: NASA / JPL-Caltech / R. Hurt (SSC-Caltech)

64 Star Formation over cosmic time

65 Star Formation over cosmic time The peak of star formation was z~1-3

66 Star Formation over cosmic time The peak of star formation was z~1-3

67 Star Formation over cosmic time The peak of star formation was z~1-3

68 Star Formation over cosmic time Kruijssen & Longmore 2013

69 The Milky Way Laboratory Stop 3: Extreme SF in our Galactic Center Figure Credit: NASA / JPL-Caltech / R. Hurt (SSC-Caltech)

70 Extreme Star Formation N(H 2 ) 70 μm 8 μm 24 μm 8 μm 4.5 μm

71 Extreme Star Formation Δv ~ 10x higher n ~ x higher High temperatures, ubiquitous exotic molecules 100 pc N(H 2 ) 70 μm 8 μm The Central Molecular Zone: CMZ N(H 2 ) from HiGAL Battersby+, in prep., 70 μm from HiGAL, Molinari+ 2011, 8 μm from GLIMPSE (Benjamin+ 2003)

72 Basic Science Questions: N(H 2 ) 70 μm 8 μm 1) What is the cause of the extremely low star formation efficiency (given the reservoir of dense gas) in the CMZ? 2) Is there an energy and SF cycle in the CMZ? Where does gas enter the CMZ? 3) Is SF induced by tidal compression by SgrA*? 4) Can we find precursors to the most massive stars in the Galaxy?

73 Central Molecular Zone Bricklet D 300 light years N(H 2 ) 70 μm 8 μm Cold dust submillimeter

74 SMA Legacy Survey of the Central Molecular Zone Long wavelength + high angular resolution detect early star formation First survey of the CMZ ever to be able to do so!

75 SMA Legacy Survey of the Central Molecular Zone Long wavelength + high angular resolution detect early star formation First survey of the CMZ ever to be able to do so!

76 CMZoom 230 GHz (1.3 mm) 240 arcmin 2 (above N(H 2 ) = cm -2 or 3x10 22 cm -2 ) 4 (0.2 pc) resolution, Δv~1.1 km/s dust continuum + spectral lines (H 2 CO, 12 CO, 13 CO, C 18 O, SiO, CH 3 OH, CH 3 CN, etc.): 8 GHz bandwidth 3 mjy RMS continuum, 0.4 K 500 hours (50 subcompact, 450 compact/custom) Complement with single-dish (APEX, CSO) observations

77 CMZoom 230 GHz (1.3 mm) 240 arcmin 2 (above N(H 2 ) = cm -2 or 3x10 22 cm -2 ) 4 (0.2 pc) resolution, Δv~1.1 km/s dust continuum + spectral lines (H 2 CO, 12 CO, 13 CO, C 18 O, SiO, CH 3 OH, CH 3 CN, etc.): 8 GHz bandwidth 3 mjy RMS continuum, 0.4 K Find star formation! 500 hours (50 subcompact, 450 compact/custom) Complement with single-dish (APEX, CSO) observations

78 CMZoom Team: CfA: Cara Battersby, Eric Keto, Qizhou Zhang, Xing Walker Lu, Mark Graham (Southampton), Nimesh Patel, Volker Tolls, Dennis Lee, Jimmy Castaño, Liz Gehret Bonn: Jens Kauffmann, Thushara Pillai University of Colorado, Boulder: John Bally Liverpool: Steve Longmore, Daniel Walker, Jonny Henshaw MPA: Diederik Kruijssen ESO: Adam Ginsburg, Katharina Immer Peking University: Luis C. Ho, NRAO: Betsy Mills

79 Basic Science Questions: N(H 2 ) 70 μm 8 μm 1) What is the cause of the extremely low star formation efficiency (given the reservoir of dense gas) in the CMZ? 2) Is there an energy and SF cycle in the CMZ? Where does gas enter the CMZ? 3) Is SF induced by tidal compression by SgrA*? 4) Can we find precursors to the most massive stars in the Galaxy?

80 Basic Science Questions: N(H 2 ) 70 μm 8 μm 1) What is the cause of the extremely low star formation efficiency (given the reservoir of dense gas) in the CMZ? 2) Is there an energy and SF cycle in the CMZ? Where does gas enter the CMZ? 3) Is SF induced by tidal compression by SgrA*? 4) Can we find precursors to the most massive stars in the Galaxy?

81 100 pc N(H 2 ) 70 μm 8 μm

82 100 pc N(H 2 ) 70 μm 8 μm Longmore et al. (2013b) The Molinari Ring (Molinari+2011)

83 100 pc N(H 2 ) 70 μm 8 μm New orbital models (Kruijssen, Dale, & Longmore 2015)

84 100 pc N(H 2 ) 70 μm 8 μm New orbital models (Kruijssen, Dale, & Longmore 2015)

85 Tidal compression of clouds N(H 2 ) from HiGAL Battersby+, in prep., 70 μm from HiGAL, Molinari+ 2011, 8 μm from GLIMPSE (Benjamin+ 2003)

86 Tidal compression of clouds N(H 2 ) from HiGAL Battersby+, in prep., 70 μm from HiGAL, Molinari+ 2011, 8 μm from GLIMPSE (Benjamin+ 2003)

87 Tidal compression of clouds Kruijssen, Dale, Longmore 2015 N(H 2 ) from HiGAL Battersby+, in prep., 70 μm from HiGAL, Molinari+ 2011, 8 μm from GLIMPSE (Benjamin+ 2003)

88 Tidal compression of clouds N(H 2 ) from HiGAL Battersby+, in prep., 70 μm from HiGAL, Molinari+ 2011, 8 μm from GLIMPSE (Benjamin+ 2003)

89 Dan Walker PhD student in Liverpool SAO Pre-doc N(H 2 ) from HiGAL Battersby+, in prep., 70 μm from HiGAL, Molinari+ 2011, 8 μm from GLIMPSE (Benjamin+ 2003)

90 Tidal compression of clouds N(H 2 ) from HiGAL Battersby+, in prep., 70 μm from HiGAL, Molinari+ 2011, 8 μm from GLIMPSE (Benjamin+ 2003)

91 70 μm 8 μm N(H 2 ) SMA 1.3mm contours ALMA 3mm contours, Rathborne+ 2014; 2015

92 70 μm 8 μm N(H 2 ) SMA 1.3mm contours ALMA 3mm contours, Rathborne+ 2014; 2015 SMA 1.3mm contours

93 70 μm 8 μm N(H 2 ) SMA 1.3mm contours ALMA 3mm contours, Rathborne+ 2014; 2015 N ff = 0.61 No SF tracers N ff = 0.65 H 2 O maser N ff = 1.28 H 2 O and CH 3 OH masers N ff = 1.76 H 2 O and CH 3 OH masers + 70 μm

94 Basic Science Questions: N(H 2 ) 70 μm 8 μm 1) What is the cause of the extremely low star formation efficiency (given the reservoir of dense gas) in the CMZ? 2) Is there an energy and SF cycle in the CMZ? Where does gas enter the CMZ? 3) Is SF induced by tidal compression by SgrA*? 4) Can we find precursors to the most massive stars in the Galaxy?

95 Basic Science Questions: N(H 2 ) 70 μm 8 μm 1) What is the cause of the extremely low star formation efficiency (given the reservoir of dense gas) in the CMZ? 2) Is there an energy and SF cycle in the CMZ? Where does gas enter the CMZ? 3) Is SF induced by tidal compression by SgrA*? 4) Can we find precursors to the most massive stars in the Galaxy?

96 Where is the Galactic Center? Map of Galaxy in a Star Formation Tracer (water maser) HOPS: A. Walsh

97 Where is the Galactic Center? Map of Galaxy in a Star Formation Tracer (water maser) Map of Galaxy in Dense Gas (HC 3 N) HOPS: A. Walsh

98 Why is the SFR low in the CMZ? Krumholz & Kruijssen 2015 Torrey et al., submitted

99 Why is the SFR low in the CMZ? N(H 2 ) from HiGAL Battersby+, in prep., 70 μm from HiGAL, Molinari+ 2011, 8 μm from GLIMPSE (Benjamin+ 2003)

100 Why is the SFR low in the CMZ? N(H 2 ) 70 μm 8 μm Mark Graham SAO Pre-doc, now a PhD student at Oxford

101 Why is the SFR low in the CMZ? N(H 2 ) 70 μm 8 μm

102 Why is the SFR low in the CMZ? N(H 2 ), 70 μm, 8 μm SMA 1.3 mm continuum

103 Why is the SFR low in the CMZ? N(H 2 ), 70 μm, 8 μm SMA 1.3 mm continuum

104 Why is the SFR low in the CMZ? 3p c The Three Little Pigs: Very similar global properties but vastly different substructure N(H 2 ), 70 μm, 8 μm SMA 1.3 mm continuum Mass ~ 3 x10 4 M T dust ~20K N(H 2 ) peak ~ 2x10 23 cm -2 Δv ~ 10 km/s Battersby, Bally, Longmore, in prep.

105 Why is the SFR low in the CMZ? 3p c N(H 2 ), 70 μm, 8 μm SMA 1.3 mm continuum

106 Why is the SFR low in the CMZ? SMA 1.3 mm dust continuum Is it star forming? Dense gas Shocked, highly excited gas Virial ratio < 2 Power-law tail in N-PDF Outflow or localized hotcore chemistry

107 Why is the SFR low in the CMZ? SMA 1.3 mm dust continuum Is it star forming? Dense gas Shocked, highly excited gas Virial ratio < 2 Power-law tail in N-PDF Outflow or localized hotcore chemistry

108 Why is the SFR low in the CMZ? SMA 1.3 mm dust continuum Is it star forming? Dense gas Shocked, highly excited gas Virial ratio < 2 Power-law tail in N-PDF Outflow or localized hotcore chemistry

109 Why is the SFR low in the CMZ? SMA 1.3 mm dust continuum Dendrograms, e.g. Shetty et al. 2012, Rosolowsky et al Liz Gehret SAO REU student

110 Why is the SFR low in the CMZ? SMA 1.3 mm dust continuum Shetty et al. 2012, see also Rosolowsky et al. 2008

111 Why is the SFR low in the CMZ? SMA 1.3 mm dust continuum Is it star forming? Dense gas Shocked, highly excited gas X Virial ratio < 2 Power-law tail in N-PDF Outflow or localized hotcore chemistry

112 Why is the SFR low in the CMZ? SMA 1.3 mm dust continuum Is it star forming? Dense gas Shocked, highly excited gas X Virial ratio < 2 Power-law tail in N-PDF Outflow or localized hotcore chemistry 3σ

113 Why is the SFR low in the CMZ? SMA 1.3 mm dust continuum Is it star forming? Dense gas Shocked, highly excited gas X Virial ratio < 2 X Power-law tail in N-PDF X Outflow or localized hotcore chemistry 3σ

114

115 Precursors to Massive Stars A B Preliminary Core mass estimates, assuming 20 K A: 550 M B: 340 M C: 140 M D: 130 M C D N(H 2 ) 70 μm 8 μm Battersby, Graham, et al., in prep.

116 Precursors to Massive Stars SMA 1.3 mm dust continuum Is it star forming? Dense gas Shocked, highly excited gas Virial ratio < 2 Power-law tail in N-PDF Outflow or localized hotcore chemistry Battersby, Graham, et al., in prep.

117 Precursors to Massive Stars SMA 1.3 mm dust continuum Is it star forming? Dense gas Shocked, highly excited gas Virial ratio < 2 Power-law tail in N-PDF Outflow or localized hotcore chemistry Battersby, Graham, et al., in prep.

118 Precursors to Massive Stars SMA 1.3 mm dust continuum Lada et al. (2010) critical density 3σ Is it star forming? Dense gas Shocked, highly excited gas Virial ratio < 2 Power-law tail in N-PDF Outflow or localized hotcore chemistry No star Formation Star Formation Battersby, Graham, et al., in prep.

119 Driving Science Questions: 1) What is the cause of the extremely low star formation efficiency (given the reservoir of dense gas) in the CMZ? High levels of turbulence are important 2) Is there an energy and SF cycle in the CMZ? Where does gas enter the CMZ? 3) Is SF induced by tidal compression by SgrA*? Observations are consistent with this scenario 4) Can we find precursors to the most massive stars in the Galaxy? We have some good candidates N(H 2 ) 70 μm 8 μm

120 H 2 CO (3-2) Lu, Zhang, et al mm dust 1.3 mm dust

121 The Milky Way Laboratory Stop 1: The Skeleton of the Milky Way Stop 3: Extreme SF in our Galactic Center Stop 2: Massive star and cluster formation

The Milky Way Laboratory Stop 1: The Skeleton of the Milky Way: We

of the Milky Way Stop 2: Massive star and cluster formation:

Stop 3: Extreme SF in our Galactic Center: new, large survey shows

122 The Milky Way Laboratory Stop 1: The Skeleton of the Milky Way: We are tracing our Galaxy with long, skinny clouds called the Bones of the Milky Way Stop 2: Massive star and cluster formation: clusters grow as the stars form! Stop 3: Extreme SF in our Galactic Center: new, large survey shows turbulence can prevent SF, tidal compression can trigger it, and it can happen where we least expect it.

Protoclusters in the Milky Way: Physical properties of massive starless & star-forming clumps from the BGPS. Brian Svoboda (Arizona)

Protoclusters in the Milky Way: Physical properties of massive starless & star-forming clumps from the BGPS Brian Svoboda (Arizona) Cygnus X in BGPS & WISE Image Credit: Adam Ginsburg Y. Shirley (Arizona)