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