1212CO(1-0) emission in CO(1-0) emission in the Magellanic Clouds, the Magellanic Clouds,

according to Mopraaccording to Mopra(Also starring the Magellanic Bridge…)(Also starring the Magellanic Bridge…)

Erik MullerErik Muller

ATNF/CSIROATNF/CSIROCollaborators so far: Collaborators so far:

Juergen Ott (PI, ATNF), Annie Hughes Juergen Ott (PI, ATNF), Annie Hughes (Swinburne), Tony Wong (ATNF/UNSW), (Swinburne), Tony Wong (ATNF/UNSW),

Jorge Pineda (Bonn) and more. Jorge Pineda (Bonn) and more.

Why CO in the Mag. Clouds?Why CO in the Mag. Clouds?

►1212CO(1-0) is a tracer for lower-density CO(1-0) is a tracer for lower-density molecular gas - signpost for SF.molecular gas - signpost for SF.

►MCs are nearby (50-60 kpc) & have MCs are nearby (50-60 kpc) & have very low metallicities very low metallicities (LMC=0.5 Z(LMC=0.5 Zsolsol, SMC = 0.1 Z, SMC = 0.1 Zsolsol) , ) , Emulate conditions as they were in the Emulate conditions as they were in the

early universe?early universe?

Technical…Technical…► Observation strategy:Observation strategy:

Observe ~5x5 amin Observe ~5x5 amin region in OTF mode (RA - region in OTF mode (RA - direction)direction)

► CO(1-0) (115.271 GHz)CO(1-0) (115.271 GHz)► ~1.75 hrs per area ~1.75 hrs per area

BW~64 MHzBW~64 MHz ΔΔV = ~0.16 Km/s V = ~0.16 Km/s RMS~0.4 K (before RMS~0.4 K (before

smoothing)smoothing)

► Tsys @115 GHz ~>400 Tsys @115 GHz ~>400 KK

SMC: SW SF region.SMC: SW SF region.

Spitzer data: Bolatto et al. 2005 (Priv. Comm)

SMC: CO according to SMC: CO according to NANTENNANTEN

Nanten 12CO(1-0) overlaid on SERC-J.

Mizuno et al, 2001

N84

N27

N66

N12

CO

SMC: SMC: 1212CO(1-0)CO(1-0)CO + NANTENRubio et al, 1993a, 1993b,1996

Latest result, smoothed to 90 asec, rebinned in velocity to ~0.5km/s, 3sig clip.

CO

SMC: SMC: 1212CO(1-0)CO(1-0)

N27/LIRS 49N12/LIRS 36

N25/26

N21/23

Latest result, smoothed to 90 asec, rebinned in velocity to ~0.5km/s, 3sig clip.

??

SMC B1#1Data is ‘first pass’ only.Very noisy!

Only three peaks appear where ICO>5sig!

Need deeper observations…

SMC: SMC: 1212CO(1-0)CO(1-0)

Rubio et al, 1993a, 1993b, Rubio et al, 1993a, 1993b,

1996 (1996 (θθ~43”)~43”)MX002 (MX002 (θθ~25”) ~25”)

- fit by eye.- fit by eye.

LIRS 49LIRS 49 V=114.6, V=114.6, ΔΔV=5.2 , V=5.2 ,

Tmb=1.99 ITmb=1.99 ICOCO=11.0, R=11.0, Rcc~16.7 ~16.7 pcpc

MMVIRVIR=8.9 10=8.9 104 4 (M (Msolsol))**

V=115, V=115, ΔΔV=~4V=~4±1.6±1.6 , ,

Tmb=~1.6Tmb=~1.6±0.4,.±0.4,. I ICOCO=6.4=6.4±3, ±3, RRcc~13~13

MMVIRVIR~5.2x10~5.2x104 4 (M(Msolsol) ) (!)(!)

LIRS 36LIRS 36 V=126.1, V=126.1, ΔΔV=3.4 , V=3.4 ,

Tmb=2.32 ITmb=2.32 ICOCO=8.45, R=8.45, Rcc~18.6~18.6

MMVIRVIR=1.2 10=1.2 105 5 (M (Msolsol) ) **

V=126, V=126, ΔΔV=3 V=3 ±1.6±1.6 , ,

Tmb=2.23 Tmb=2.23 ±0.4±0.4 I ICOCO=6.7 =6.7 ± 4, R± 4, Rcc~ ~ 15 pc15 pc

MMVIRVIR~3.3x10~3.3x104 4 (M(Msolsol) ) (!)(!)

New Mopra Results are generally consistent with the literature.

“Clumpfind” does not perform well with noisy data.

Using alternatives…

SMC: SMC: 1212CO(1-0), HCO(1-0), HIICO

N27/LIRS 49N12/LIRS 36

N25/26

N21/23

??

SMC B1#1

HI (1/25)CO

• APEX, high order transitions of CO (4-3) •Comparable resolutions to Mopra

• ASTE observations are underway (U Nagoya)

SMC: ASTE/APEX SMC: ASTE/APEX

Contours: APEX CO(4-3) transition.Background image: 2MASS J band – (UMASS/IPAC)

• ICO, Tmb are much lower for SMC than for LMC (can be x ~10!)

• Cloud radii are much smaller in SMC than for LMC• More exact quantifiction of ‘much smaller’ pending less noisy results •~Rlmc/Rsmc ~2-3 for brightest clouds).•ΔVlmc/ ΔVsmc ~2

•Mvirlmc/Mvirsmc ~ 8-12 (or more..)

LMC, SMC: LMC, SMC: 1212CO(1-0)CO(1-0)

Hα

SMC: CO, HSMC: CO, HααCO

N27/LIRS 49 N12/LIRS 36

N25/26

N21/23

SMC. Where to with Mopra?SMC. Where to with Mopra?

• Continue to fully sample SW area with Mopra? • Multi wavelength obs for N88/N66 ?• ASTE @ CO(3-2) has comparable resolution to Mopra @ CO(1-0)

• Other regions in SMC?• Existing CO(1-0) (and (2-1)) data for N66 are small field and mostly under sampled

•Dense core tracers (or ATCA? E.g. Muller+Ott in prep. HCO+, HCN)