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The Maryland-Magellan Tunable Filter
S. Veilleux (U. Maryland)
http://www.astro.umd.edu/~veilleux/mmtf
Magellan = Arizona, Carnegie, Harvard, Michigan, MIT + Chile
PLAN
General principles
Prototype: TTF (Taurus Tunable Filter) Description
Science
MMTF Description
Commissioning
Science
Outlook
Optical Fabry-Perot Interferometer
Etalon: two parallel flat semi-transparent mirrors separated by a fixed distance L
This system acts as a narrow-band filter, producing concentric rings at each wavelength
m = 2 L cos 2mono ~ 2 / (N m) (N = finesse) (m = few – 150)
Etalon
Search for Starburst-Driven Winds
• Star-forming disk has [N II] 6583/H < 1
• Shocked wind material has [N II] 6583/H > 1
(SV & Rupke 2002)[N II] 6583/H
H 6563 [N II] 6583
[N II] / H
1 kpc
Disk Wind
NGC 1482
TTF Imaging
5 kpc
“Zone of Influence” of Winds in Local Starbursts
• Warm ionized gas from superwinds has been detected out to ~ 10 – 30+ kpc from the nucleus [bounded by sensitivity of instrument]
NGC 1482: H + [N II] + X-rays
12 kpc
wind
disk
10 kpc
[NII]/H NGC 1482
(SV, et al. 2003)
“Zone of Influence” of AGN–driven Winds
• AGN-driven winds clear out path for ionizing radiation “ionization cones” on large scale
(Optical: SV et al. 2003; HI: Brinks 2003; X-ray: Young, Wilson, & Shopbell 2001)
NGC 1068 log(H) + HI 21-cm
10 kpc
NN
log([O III]) + X-rays
10 kpc
Maryland-Magellan Tunable Filter ( )
PI: S. Veilleux (U. Maryland) Co-PIs: J. Bland-Hawthorn (USyd), A. Dressler (OCIW), M. Rauch (OCIW),
& S. Vogel (U. Maryland) Co-Is: B. Bigelow (OCIW / U. Michigan), M. McDonald (Maryland), D. Rupke
(Maryland), P. Shopbell (Caltech), B. Sutin (OCIW/Skewray), I. Thompson (OCIW), B. Weiner (Arizona), & R. Weymann (OCIW)
Additional Technical Support (OCIW): A. Bagish, C. Birk, T. Hare, D. Osip, F. Perez, A. Uomoto
Funding Agency: NSF/ATI (instrument), NSF/EXC (science)
Tunable filter for IMACS on the Baade 6.5m telescope with wavelength coverage ~ 5000 – 9200+ Å, bandwidth ~ 6 – 20 Å, and FOV ~ 27
Resolution versus FOV
R
FOV 105 106
100
1000 MMTF
Others
MMTF: Schedule
August 15, 2003: NSF/ATI Award notification
Shipment: End-Result of Attempt #1
MMTF: Schedule
August 15, 2003: NSF/ATI Award notification
June 2006: Commissioning & first light
Semester 07A: PI instrument
Semester 09A: Facility instrument
MMTF: Description Host instrument: IMACS
• FOV: 27• DIQ: ~ 0.4 – 0.7• NEW CCD: 8 x E2V 2048 x 4096
x 15 m pixels
Low-order Fabry-Perot etalon: • Etalon: IC Optical Systems ET-
150-FS-100, 150 mm, /100
• Finesse: ~ 30 (effective)
• Broad-band coating: ~ 5000 – 9200+ Å
• Bandwidth: ~ 6 – 20 Å
• Monochromatic FOV: ≤ 12' @ 6600 Å
Electronic controller: • T-stabilized & remote-controlled
Order-blocking filters (R ~ 30)
New CCD
Etalon ET-150
MMTF: Observing Modes Mode #1: stare mode
• fixed-gap narrow-band imaging over whole FOV Mode #2: gap scanning mode
• low-resolution data cube Mode #3: charge shuffling & frequency switching mode
• The charges on each CCD are shuffled up and down at the same rate that the etalon plates are scanned between two / three discrete gap positions
• FOV ~ 2 x 4.5 x 27 ~ 250 �• Need two telescope nods of 4.5 for contiguous FOV
Mode #2 Mode #3
Commissioning (June 2006)
Successful Commissioning (June 2006) !
MMTF Commissioning
900-sec Hα “snapshot”
Full Moon!
NGC 4945
┼N
E
MMTF Commissioning
900-sec Hα “snapshot”
Full Moon!
Cen A
┼N
E
MMTF Commissioning
Cen A
900-sec [N II] λ6583 “snapshot”
Full Moon!
┼E
NN
MMTF Commissioning
Cen A jet
900-sec “snapshot” of jet in Hα
Full Moon!
← 145” →
←
170
”
→
60’’ = 1 kpc
┼E
N
Cen A
FUV GALEX + R-band
→ Jet-induced star formation
Recently: Deep emission line maps to compare with GALEX data
N
┼E (Cackett et al.)
MMTF Commissioning
NGC 1313– SB(s)d
– z = 0.0016
– [N II] / Hα = 0.1 → 0.7
Hα [N II]
[N II]/Hα
0 1
← 280” →
(Weiner et al.)
[Veilleux et al. 1999]
┼
N
E ← 780” →
Emission-Line Imaging of Nearby Galaxies
NGC 5713– SAB(rs)bc pec
– z = 0.0063
– SINGS galaxy
– 10 + 20 min
– [N II] / Hα = 0.3 → 0.7
10
Hα [N II]
[N II]/Hα ← 140” →
(Weiner et al.)
┼
N
E
← 300” →
MMTF Science
Surveys of emission-line galaxies (& nebulae) at low- and high-z in the field, cluster, supercluster environments
5-σ sensitivity (2” aperture): ~ 1 x 10-17 erg s-1 cm-2 in 1 hr @ 6600 Å
0 0.5 1.0 1.5 2.0
10 Mo/yr
1 Mo/yr
10 Mo/yr
1 Mo/yr
0.1 Mo/yr
10 Mo/yr Galaxy 1 Mo/yr LMC 0.1 Mo/yr SMC
–
18
–16
–14
–12
[O II]
Ly
Cooling Flow Clusters
object
(McDonald et al.)
Cooling Flow Clusters
object
(McDonald et al.)
Supercluster @ z = 0.73 in the COSMOS Field
object
(Scoville et al. 2007)
“Tomography” of z = 0.73 Supercluster in the COSMOS Field
~15 minutes / slice x 14 slices (Veilleux et al.)
Damped Lyα Galaxies
DLA:– z = 4.38 → λ = 6543.8 Å– FWHM ~ 9 Å– Factor 5x reduction in QSO light– No 3-σ detection within 1 ”
~2 x 10-18 erg s-1 cm-2
SFR < 0.6 Msun / yr (~LMC)
56 kpc
QSO 1202-0725:– z = 4.7
(Rauch & Becker)
MMTF: Science
Emission-line imaging of galactic nebulae
Deep multi-line imaging of nearby galaxies
Survey of emission-line galaxies & nebulae at low- and high-redshifts in the field, cluster and supercluster environments
PI Instrument: 9 programs, 16 nights
http://www.astro.umd.edu/~veilleux/mmtf
5-σ sensitivity (2” aperture): ~ 1 x 10-17 erg s-1 cm-2 in 1 hr @ 6600 Å
http://www.astro.umd.edu/~veilleux/mmtf
http://www.astro.umd.edu/~veilleux/mmtf
http://www.astro.umd.edu/~veilleux/mmtf
http://www.astro.umd.edu/~veilleux/mmtf
http://www.astro.umd.edu/~veilleux/mmtf
MMTF
Proposals & collaborations welcome!
