stars M - ESO

Head: Thomas Preibisch
Postdocs: Thorsten Ratzka 1
PhD
Students:
Paola Mucciarelli 2
Veronica Roccatagliata 3
Miwa Goto 4
Talk
Nick Moeckel (06/2012)
Rebekka Grellmann 5
Stephanie Pekruhl 6
Henrike Ohlendorf 7
Judith Ngoumou 8
Frauke Alexander 9
Talk
Talk
Benjamin Gaczkowski 10
3
4
9
10
Ludwig-Maximilians-
Universität München
Universitäts-Sternwarte
5
6
1 2
7
8

X-ray observations of
star forming regions
Paola Mucciarelli
Frauke Alexander
Chandra
Spitzer
Talk
S255-257

Infrared Interferometry
Protoplanetary Disks
1 AU
Thorsten Ratzka Talk
Rebekka Grellmann
SB
(0.13
AU)
θ 1 D
IOTA
�
�
0.02’’
Stellar Multiplicity
B1
0.5’’
B4
B2 – B3:
ρ = 0.117"
B2
B3
D1 – D2:
ρ = 0.0184"
HST image
Bally et al. (1998)
1’’
θ 1 B
θ 1 C
SB
(1 AU)
0.025’’
A1 – A2:
ρ = 0.215"
C1
θ 1 E
θ 1 A
C2
C1 – C2: ρ = 0.024"
A2
A1
Herbig &
Griffin 2006
SB
(0.2 AU)
0.1’’

A panchromatic view
of massive star feedback
& triggered star formation
in the Carina Nebula
●Thorsten Ratzka
●Veronica
Roccatagliata
● Stephanie Pekruhl
Talk
● Henrike Ohlendorf
● Judith Ngoumou
● Benjamin
Gaczkowski
Herschel far-infrared
X-ray
HAWK-I near-infrared
LABOCA sub-mm

η Car
the galaxy's most
luminous star
The Great Nebula in Carina
Tr 16
Tr 15
+ 70 O + WR stars (M ✶,max ~ 120 M ⊙ )
Tr 14
D = 2.3 kpc
15 '
10 pc
Orion Nebula
at the same
physical scale

Orion Nebula
2 O stars
M ✶,max = 36 M ⊙
Carina Nebula
70 O+WR stars
M ✶,max ~ 120 M ⊙
close enough to study low-mass stars
1'' = 420 AU = 0.002 pc
1'' = 2300 AU = 0.01 pc
30 Doradus
~1000 O stars
M ✶,max ~ 150 M ⊙
large enough to sample the top of the IMF
1'' = 52 000 AU = 0.25 pc
Carina is the best bridge between
detailed studies of nearby regions and
more massive but more distant extragalactic starburst regions

Zoom into the central region: N
η Car
~ 120 M ⊙
log L = 6.67 L ⊙
P wind = 30 000 L ⊙
© ESO images
Tr 16
Tr 14
WR 25 ≥ 70 M ⊙ , log L = 6.22 L ⊙ , P wind = 5100 L ⊙
HD 93129A O3Ia, ≥ 100 M ⊙
log L = 6.17 L ⊙ , P wind = 7000 L ⊙
Until ~ 2010: Carina Nebula = “cluster of clusters”
Feinstein 1995: estimated total population of ~ 7000 stars

Revealing the young stellar population: HAWK-I near-infrared survey
600 336 infrared sources in Carina Nebula
Preibisch et al. 2011, A&A 530,A43
Edge-on disk
Preibisch et al.
2011,
A&A 530, A40
J-H-K s composite of the central part
→ Carina Nebula contains ~ 60 000 young stars

Identifying the young stellar population:
The Chandra Carina Complex Project
● 14 368 X-ray point sources
● 10 714 Carina members
The first unbiased sample of the
low-mass stellar population.
≥ 80% (50%) complete at ~ 1 M ⊙ (0.5 M ⊙ )
- 50% of the YSOs in clusters
- 50% YSO widely distributed
→ no “cluster of clusters”,
but an association
● Diffuse X-ray emission
Stellar winds (+ supernovae ?)
have filled the super-bubble
with hot plasma.
PI: Leisa Townsley (Penn State)
CCCP Special Issue
Vol. 194, May 2011

Spitzer IRAC map
3.6, 4.5, 8.0 μm
shows cloud surfaces
+ YSOs
Treasure Chest
HAWK-I J, H, K
Many dust columns contain
young stellar objects
in their heads
Smith et al. 2010:
Scenario of triggered star formation

Investigation of the
Molecular Clouds
Step 1:
LABOCA 870 μm
survey
● Total dense cloud mass:
~ 60 000 M⊙ Preibisch et al. 2011,
A&A 525, A92
LABOCA + optical

Investigation of the
Molecular Clouds
Step 2:
Herschel
70 – 500 μm
survey
● Total
cloud mass:
≥ 600 000 M ⊙
Preibisch et al. 2012,
A&A in press
arXiv 1204:0627
optical
+
Herschel 70
+
Herschel 350

Detailed studies of pillars Herschel temperature map
Spitzer + LABOCA: 3.6 + 8 + 870 μm
Recent APEX line observations:
12 CO 7-6, 12 CO 6-5, 12 CO 4-3,
12CO 3-2, 13CO 3-2, C18O 3-2
→ gas kinematics
comparison to model predictions
Gritschneder et al. 2009, ApJ 694,L26
→
→