I want to epress my joy for:
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Transcript of I want to epress my joy for:
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I want to epress my joy for:
-sharing with you guys this time in this beatiful planet
-sharing the excitement unveiling the secret live of the stars
-sharing the friendship with Peter who opened roads to the big scenario of massive stars
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Augusto Damineli (IAGUSP)
Robert Blum (NOAO)
Peter Conti (JILA)
Elysandra Figuerêdo (Open Un.)
Alessandro Moisés (IAGUSP)
The Stellar Content of Galactic Giant HII Regions
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MellingerMellinger2MASS2MASS
Many methods indicate Sb-Sc types
Where are trhe arms? Longer wavelengths => clear view, but mixed structures
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RVs of radio recombination lines from HII regions => Distances to HII regions + rotation curve
face-on map
(l,b) coordinates
Clemens 1985
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SunHII RegionsRusseil 2003
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Radial velocities: - degenerate toward the GC line-of-sight
- 2-valued r<R
Limitations of the method:
Non-rotational components: - warm gas outflows from HII regions (10 Km/s - density-wave attractive force ( up to 10 km/s) - collisions between GMCs
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Project started ~15 years ago by Conti, Hanson, Blum…
-K-band imaging+spectra of ionizing O-type stars -Spectroscopic parallax: robust physics like in the optical window -Errors constrained by multiple stellar spectra
Giant HII Regions
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Our Method: Giant HII Regions (NLyc=>1050 ph/s =>10 O7V*) good tracers of the spiral arms
selected from radio and FIR surveys
50 imaged with Blanco/SOAR
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Colour- Magnitude Diagram:
foreground stars
ZAMS of the HIIR
Candidates for spectroscopy
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Spectroscopy of O-type stars:
Distance Module
DSpPtHanson, Conti & Rieke (1996)
Spectral Type
O6V O8V
Late O-type stars
lines used to determine the spectral type
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Id Kdist
kpcref Sppdist
kpcref
M8 2.8 R03 0.6 Bik04
W31 >4.1-12.3 C&E04 3.4 ± 0.5 BDC
M17 2.4 R03 1.3 Hans97
W42 3.7 -11.5 R03 2.2 ±0.8 BCD
W43 6.2 R03 5.9 ± 0.7 BDC
W49A 11.8 Wetal04 8.4 Bik04
W51A 5.5 R03 2.2 F07
W3OH 4.2 R03 1.95 Xu06
NGC3603* 7.9 R03 6.0 Stolte04
G282.0-1.2G298.9-0.4
5.910.4 R03
5.3 ±1.23
F05Bik04
G333.1-0.4G331.5–0.1
3.510.8
R03R03
2.4 ±0.44.5 ±0.3
F05F05
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All shifts are toward smaller distances!
Conti & Crowther 2004
Sun
GC
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Star Formation Rate in the Milky Way
Scaling the reduction to all sources
NLyC = 1.7 × 1052 ≥ 1.8 M/year
Conti & Crowther 2004NLyC = 2.4 × 1052 ≥ 2.6
M/year
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Trig. VLBA OH masers d = 1.95±0.04 kpc Xu et al. 2006
SpPht distance d = 2.2 kpc (optical) Humphreys 1978
W3OH: emblematic for distance discrepancy
Perseus arm is at wrong kinematic distance!
Kin. distance d = 4.2 kpc (RV = -45 km/s) Russeil 2003
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What is the role of the reddening law?
AK ~ 1/
Mathis (1990) =1.7 Nishiyama et al. (2006) =1.99
--Calibration uncertainty: MV = ± 0.7 Vacca et al. 1996 – Unresolved blends: 2 identical stars => Distance 40% smaller – Projected stars in the cluster line-of-sight
Limitations of the method:
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G353.19+0.64
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Ak=1
Ak=2
Ak=3
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Name DK DNish DMat kpc
M8 2.8 0.9 0.8
W31 >4.1-12.3 3.9 3.3
M17 2.4 1.7 1.6
W42 3.7-11.5 2.8 2.5
W43 6.2 6.3 4.7
W49A 11.8 14.7 11.0
W51A 5.5 4.0 3.0
G298.2-0.3 10.4 4.6 3.9
G333.1-0.4 3.5 3.3 2.4
G331.5-0.1 10.8 5.5 4.5
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--- NGC3576
The slope of the luminosity function is independent of the Galactic ambient
= 0.35 0.05
K-band Luminosity
Function
--- G333.1-0.4
SalpeterIn line with Massey 2003
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L (H) [ergs/s]= ( 1.43 ×10-12 ) NLyC [photons/s]
Conti & Crowther 2004
3GHIIR + luminous
M17
W49A
NGC3603
Morphologic Type of Milk Way
Kennicutt (1988)