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Joint DDT Program Star Formation in the Gem OB1 Region. Chris Davis, Jan Wouterloot, Watson Varricatt, Ant Chrysostomou and the JCMT/UKIRT Science staff. Molecular Clouds in Gemini Second/Third Galactic Quadrant : l ~ 190 degs (Galactic Anti-Centre) 13 CO J = 1-0 survey

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joint ddt program star formation in the gem ob1 region

Joint DDT ProgramStar Formation in the Gem OB1 Region

Chris Davis, Jan Wouterloot, Watson Varricatt, Ant Chrysostomou

and the JCMT/UKIRT Science staff

slide2
Molecular Clouds in Gemini

Second/Third Galactic Quadrant: l ~ 190 degs (Galactic Anti-Centre)

13CO J = 1-0 survey

(170 < l < 196 degs) by Kawamura et al. (1998) with a 3’ beam.

CO J = 1-0 mapping

with FCRAO with an angular resolution of about 50” (Carpenter et al. 1995)

13CO contours (Kawamura et al. 1998)

Crosses mark locations of early type stars - the OB associations - catalogued by Humphreys (1978)

slide3
Molecular Clouds in Gemini

Clouds associated with the Orion Spur or Perseus Arm? Star formation at ~ 300pc and ~ 2 kpc

Studying clouds with large galacto-centric distances…

13CO contours (Kawamura et al. 1998)

Crosses mark locations of early type stars - the OB associations - catalogued by Humphreys (1978)

slide4
Existing Complementary Data:

Near-IR: UKIDSS GPS JHK data available (WFCAM)

Mid-IR: Some Spitzer data are available in PI

projects (but also GLIMPSE360 - 3.6um and 4.5um)

Far-IR: Herschel data will eventually be available (Hi-GAL360, 5-band PACS and SPIRE)

Sub-mm: not covered by Gould Belt Survey, but is part of JPS (SCUBA-2)

MSX A

MSX A

slide5
How can we complement these existing/proposed observations?

Joint UKIRT/JCMT Project

CO 3-2 mapping with Harp/JCMT

H2 (and K band) imaging with WFCAM/UKIRT can

slide6
Infrared “Finders”

Firstly we imaged the clouds along the plane with WFCAM…

Each square represents a “WFCAM Tile” (covering 0.8 sqr degrees)

WFCAM - 0.4” pixels

K >18th mag point sources detectable in a few minutes (broad band) or ~10 mins narrow band)

scientific goals of the project
Scientific Goals of the Project

1. Map star formation on global scales, across a number of independent regions and GMCs in the outer galaxy

2. Trace jets and outflows in the near-IR (H2) and the Sub-mm (CO 3-2)

3. Identify (Spitzer) protostars from their association with outflows

4. Identify proto-stellar cores from their association with outflows

5. With combined UKIRT/Spitzer/JCMT/Herschel data, build up a census of prestellar cores, protostellar cores, and T Tauri stars (no molecular flow)

6. Establish prestellar/protostellar ratio, lifetimes, etc…

- Star formation efficiency

- Star formation rate

slide12
Tile A

1’

slide13
Tile B

1’

slide14
Tile B

1’

slide15
Tile E

1’

slide16
JCMT ObsLarger, shallow maps:CO 3-2 - 1000 MHz bandwidth - 488 kHz/0.4 km/s resoln - 0.1 sec sample time - 3/4 array step - basket weaveSmall, deep maps:CO 3-2 and H13CN 4-3 - 250 MHz bandwidth - 61 kHz/0.05 km/s resoln - 1 sec sample time - 1/4 array step - basket weave (some map pairs repeated with 15” offset).

Small maps

Tile A:

A-CenA 06:08:43.0 +21:31:06 6’ x 6'

A-Na 06:08:52.0 +21:38:09 7’ x 6'

A-Nb 06:08:32.0 +21:40:51 3’ x 3' (weak)

A-S 06:09:26.0 +21:23:30 5’ x 3' (weak)

A-NE 06:09:52.0 +21:38:26 4’ x 3' (weak)

Tile B:

B 06:08:58.0 +20:39:10 21’ x 9'

B-S 06:09:53.0 +20:32:50 9’ x 9'

B-W 06:07:47.0 +20:39:36 3’ x 3' (weak)

B-ano 06:09:08.0 +20:28:00 5’ x 5' (weak)

Tile D:

D-NE 06:14:54.0 +19:01:40 9'x5'

Tile E:

E-Cen 06:14:24.0 +17:44:30 12’ x 7'

E-W 06:13:57.0 +17:50:28 4’ x 3' (weak)

E-NW 06:13:45.0 +17:55:20 3’ x 3' (weak)

Tile F:

F-Cen 06:12:58.0 +17:57:44 20’ x 11'

slide17
Tile B - Fast Map

CO 3-2 integrated

Map size: ~ 55 x 55 arcmin

slide18
TILE A

AFGL 5180

AFGL 6366

CO 3-2 integrated intensity

slide19
AFGL 5180

TILE B

Sh 2-252 A

AFGL 5183

AFGL 6366

CO 3-2 integrated intensity

slide20
AFGL 5180

Sh 2-255B

TILE F

Sh 2-255

AFGL 6366

TILE E

CO 3-2 integrated intensity

co 3 2 data quality
CO 3-2 data quality…

Large, shallow maps - 0.4 km/s resolution :

0.6-1.2 K in most regions (as high as 1.8 K in some parts of Tile A, and up to 3.0 K in parts of Tile E)

Small, deeper maps - 0.05 km/s resolution:

0.6-0.9 K in almost all regions (more even depth)

We are currently focusing on Tile E

slide22
Tile E

H2-K image

Outflows Identified independently by manually scanning through PV diagrams (binned to 0.55 km/s resolution)

slide23
Tile E

Outflow #19

slide24
Tile E

H2-K image

Bipolar Outflow #3 and 5

slide26
Antonio’s Outflow Extraction Algorythm!

Calculates moments V and sigma from average spectra (excluding brightest spectra) and integrates between 2 and 15 sigma either side of this average V.

Remo also has a script!

Color-composite of red-shifted, ambient (green) and blue-shifted CO

HV Red- and Blue-shifted contours

on “ambient velocity” CO image

slide28
H2-K Image

SCUBA contours

SCUBA 850 micron contours (Di Francesco et al. - SCUBA archive paper)

Plenty of dust emission … “protostellar” cores clearly related to outflows

final remarks
Final Remarks

1. We have identified a very interesting region.

2. Complementary data are available in abundance.

3. The DDT project doesn’t “tread on the toes” of exisiting surveys.

4. Possibility for a number of “stand alone” papers (examining individual regions) and/or an “overview” paper comparing these seemingly similar sites of clustered star formation.

5. JCMT and UKIRT scientists are now collaborating (best chums) !

6. …

slide30
Tile B

Thank You

Spitzer - IRAC

3.6/4.5/5.8 micron

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