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November 14, 2007 CTIO-Gemini Colloquium, La Serena 1
Slicing Up Galactic HII Regions with
NIFS
and...
The Incredible Shrinking Milky Way
R. BlumNOAO Gemini Science Center, Tucson
Peter Conti (JILA, University of Colorado) Augusto Damineli (IAG, University of São
Paulo) Elysandra Figuerêdo (Open University,
London) Cássio Barbosa (UNIVAP, Brazil) Alessandro Moisés (IAG, University of São
Paulo)
Collaborators
Galactic Structure
Galactic Structure
MellingerMellinger2MASS2MASS
Galactic Structure
Galactic Structure
Russeil et al. (2007)Russeil et al. (2007)
Galactic Structure
Russeil et al. (2007)Russeil et al. (2007)
RRL can exhibit non circular motions
Use spectrophotometric distances instead
NIR, lower extinction (but RJ tail)
Need good Mbol, spectral standards
Survey ~ 50 GHII on Blanco/SOAR
W31
Blum et al. (2001)Blum et al. (2001)
W31
Blum et al. (2001)Blum et al. (2001)
H-KJ
-HH-K
K
W31
Blum et al. (2001)Blum et al. (2001)
Sun
GC
``A Smaller Milky Way''
Dozen GHII
Hanson et al., Bik
Xu et al., W3(OH)
What is source of
difference?
Figure courtesy A. Damineli
.Figure courtesy ADamineli
HII Luminosity Function (NLyC)
Smith & Kennicutt 1989
Galaxy H-type
M33 Scd -2.3
M81 Sab -2.1
LMC Irr -1.7
Sbc-Sc -2.0
Milky Way -2.2
This work
Milky Way = -2.0
Figure courtesy A. Damineli
.Figure courtesy ADamineli
Galaxy Type
Milky Way
Smith & Kennicutt 1989
Figure courtesy A. Damineli
.Figure courtesy ADamineli
W49 FBright UCHII (Welch, DePree)
W49 spectra courtesy of Tom Geballe, UKIRT
Blum et al. (2004)Blum et al. (2004)
Phoenix/Gemini SouthConsistent with early B-type, lateO type, largeK excess
CO Emission Sources
Blum et al. (2004)Blum et al. (2004)
Massive Young Stellar Objects (MYSO, UCHII, HCHII)
November 14, 2007 CTIO-Gemini Colloquium, La Serena 17
NIFS/Altair Observations
GT observations w/Peter McGregor
Barbosa et al. 2007A
Search for ionizing sources of Galactic HII
regions (massive stars, distances)
Testing NIFS modes in crowded fields, high S/N
weak features
UCHII regions
November 14, 2007 CTIO-Gemini Colloquium, La Serena 18
NIFS/Altair Observations
K-band Arc
60 0.05'' pixels
29 0.1'' slices
November 14, 2007 CTIO-Gemini Colloquium, La Serena 19
G45.45-0.06
Feldt et al. (1998)Feldt et al. (1998)
November 14, 2007 CTIO-Gemini Colloquium, La Serena 20
G45.45-0.06, Line Maps
November 14, 2007 CTIO-Gemini Colloquium, La Serena 21
G45.45-0.06, Spectra
November 14, 2007 CTIO-Gemini Colloquium, La Serena 22
G45.45-0.06, Spectra
November 14, 2007 CTIO-Gemini Colloquium, La Serena 23
Unidentified IR Lines
Geballe et al. (1991)
PNe show lines at 2.199 um and 2.287 um
IP 30-40 eV Dinnerstein 2001
[Kr III], [Se IV]
HII regions too
November 14, 2007 CTIO-Gemini Colloquium, La Serena 24
G5.89-0.39
Feldt et al. (1999)Feldt et al. (1999)
He I
H2
[FeIII]
?
H2
November 14, 2007 CTIO-Gemini Colloquium, La Serena 25
G5.89-0.39, Line Ratios
[Fe III] 2.1451um/2.2178umHe I 2.1127um/Brγ
November 14, 2007 CTIO-Gemini Colloquium, La Serena 26
G5.89-0.39 + CloudyHe I 2.1127um/Brγ Brγ / Dust
Hunter et al. (2000)Hunter et al. (2000)
November 14, 2007 CTIO-Gemini Colloquium, La Serena 27
W51 A
Part of W51 (~degree)
6-7 kpc
LyC ~10^51, 200 O7 V
NIR: Goldader,
Okumura
Completely obscured
at visual wavelngths
Figuerêdo et al. (2007)Figuerêdo et al. (2007)
November 14, 2007 CTIO-Gemini Colloquium, La Serena 28
W51 A
Figuerêdo et al. (2007)
NIRI Distance=2kpc
not 6-7 kpc!
November 14, 2007 CTIO-Gemini Colloquium, La Serena 29
W51 IRS2
VLT Archive image Barbosa et al. (2007)Barbosa et al. (2007)
November 14, 2007 CTIO-Gemini Colloquium, La Serena 30
W51 IRS2
Barbosa et al. (2007)Barbosa et al. (2007)
November 14, 2007 CTIO-Gemini Colloquium, La Serena 31
W51 IRS2
Lacy et al. (2007)Lacy et al. (2007)
November 14, 2007 CTIO-Gemini Colloquium, La Serena 32
W51 IRS2: [SIV]
Lacy et al. (2007)Lacy et al. (2007)
Ionized outflow from MC
November 14, 2007 CTIO-Gemini Colloquium, La Serena 33
W51 IRS2: NIFS/Altair/LGS
2.14um continuum
November 14, 2007 CTIO-Gemini Colloquium, La Serena 34
W51 IRS2: NIFS Brgamma
November 14, 2007 CTIO-Gemini Colloquium, La Serena 35
W51 IRS2: NIFS Brg channel map
November 14, 2007 CTIO-Gemini Colloquium, La Serena 36
W51 IRS2: NIFS H2
November 14, 2007 CTIO-Gemini Colloquium, La Serena 37
W51 IRS2
Maser proper motions in W51 N (1'' S of IRS2E)
Association with Lacy et al. Out flow unclear
Motion mostly in plane of sky
Fit to radial out flow: 6 kpc.
November 14, 2007 CTIO-Gemini Colloquium, La Serena 38
W51 IRS2e
MYSO
No photospheric
features
CO emission
November 14, 2007 CTIO-Gemini Colloquium, La Serena 39
IRS2W/W51d AO wins again!
Early O-type
No CIV, earliest type
One of a few of the very
youngest, most massive
stars detected (Hanson, Bik)
November 14, 2007 CTIO-Gemini Colloquium, La Serena 40
IRS2W/W51d W51d has K-band excess, so difficult to
determine the spectrophotometric distance
Max disk model: 7 kpc
All K excess model: 11 kpc
Max inclined disk: 1 kpc
Need to model SED
Size and NIR photosphere argue for 6-7 kpc
November 14, 2007 CTIO-Gemini Colloquium, La Serena 41
Summary
Picture of the inner Milky Way and spiral structure is emerging
NIFS is a powerful tool for crowded field spectroscopy
Excellent line maps, ratios Identified ionizing sources in G45.45-0.06, W51
IRS2 W51 is a complex region with multiple
components projected on the sky