Download The Galactic Center with Gemini

Early Science Results and Status
of the Gemini Telescopes
Prepared by Phil Puxley
Barolo, October 2001
Gemini North, Hawaii - 4200 m
Beginning of science operations: 2000B
Gemini South, Chile - 2900 m
Beginning of science operations: 2001B
Gemini North: Early science
with “visitor” instruments
 Why? Very late delivery of facility instruments


NIRI, GMOS and GNIRS more than 2 yrs late
Use of 2 visitor instruments
• Get some science out; shake down telescope systems and operational
processed…but very labour intensive
• The U Hawaii/NSF Adaptive Optics near IR system Hokupa’a/QUIRC
• The U Florida/NSF/NASA mid IR imager OSCIR
 Observing on Gemini North: programs

Demonstration Science (2000B)
• Galactic Center (Hokupa’a)

“Quick Start” service observing (2000B)
• Hokupa’a (26 programs) & OSCIR (10 programs) – 53 science + 68 cal CDs

Classical observing (2001A)
• 41 programs on Hokupa’a and OSCIR (on-going)

13 presentations and posters at AAS #198
Sub-arcsec IR Imaging with
Hokupa’a on Gemini North
 Hokupa’a : 36 actuators AO
system
Developed and operated by the
University of Hawaii Adaptive
Optics Group
 With support from the NSF

 QUIRC: 1k x 1k HgCdTe device
20’’ x 20’’ field with
Gemini/Hokupa’a
 JHK and narrow-band filters

Engineering
into science
M32
K’-band
20”x20”
FWHM=
0.12”
Bright *
AGB tip
K = 15.5
Small H-K color dispersion
- Brightest stars well
mixed throughout
- No evidence for radial
age gradient
Davidge et al. 2000, ApJ, 545, L89 = FIRST PAPER
The Stellar Content of the
Central Regions of M33
A.W. Stephens & J.A. Frogel
The Ohio State University
M33
pc)
(80kpc)
20”
30’ (7
M33 Core Optical-IR CMD
Luminosity Function
First results on center of M33





Complicated CMD
Range of stellar ages
LF slope steeper than bulge of our Galaxy
Disk-like stellar distribution to ~3”
No significant radial variations in LF or CMD
QSO “absorbing” galaxies
Mark Chun, Gemini Observatory
 Radio loud quasar Q2251+113
with lobes SE-NW

V ~ 15.8; DLA at z=0.11
 Hokupa’a/QUIRC
K-band: 39 min
 FWHM = 0.17”
 K(5s ) ~ 22.2

 Object to SE

K’ ~ 20.5
• K = - 18.0 if at absorber
• K = - 20.5 if near QSO
 Possibly detecting radio lobes in
the near IR
The Galactic Center with
Gemini-Hokupa’a/QUIRC
 DEMONSTRATION SCIENCE program prior to
starting community science obs: [10 half-nights run]
 Stellar content near SgrA* and Arches Cluster


Variability and Extinction maps
Creation/enlargement of a GC astrometric database
 Data product: 3.5 GB reduced and available as 60
images (250 MB) on a CD



Eleven 20”x20” fields in H and K’
6 min (K’) / 12 min (H) to 40 min per field
FWHM (H,K) = 0.08” - 0.15”
Galactic Center DS: The Team
Science definition
Vicky Alonso, Cordoba
Robert Blum, CTIO
Michael Burton, UNSW
Simon Casassus, U.Chile
Angela Cotera, Steward
Tim Davidge, HIA
Tom Geballe, Gemini
Andrea Ghez, UCLA
Fluvio Melia, Steward
Dante Minniti, U.Catolica
Mark Morris, UCLA
A. Quirrenbach, UCSD
Doug Simons, Gemini
Program Support/DR
Tim Davidge, HIA
Bob Blum, CTIO
Angela Cotera, Steward Obs.
Mark Chun, Gemini
Coordination
F.Rigaut
Instrument Specialists
Mark Chun, Gemini
Joe Jensen, Gemini
Wolgang Brandner, UH-IfA
Dan Potter, UH-IfA
Galactic Center
Demo Science
Eleven 20’’x20’’
fields
Orange symbol is
the guide star for
Hokupa’a.
Field 11 is the
Arches Cluster
Very high
extinction
clouds
IRS8 (bow shock)
Filters:
•H
•K’
•CO
•CO cont.
40”
4’
5”
Bow shock
>10 stars
per arcsec2
at K~18
>220 stars in 5”x5”
UH-88”, Courtesy W.Brandner, 0.65” seeing
Gemini N/Hokupa’a-Quirc (U of H/NSF) IRS7
SgrA*
Analysis of GC Data
Francois Rigaut, Gemini Observatory
 Gemini images probe the
GC luminosity function
2.5 mag deeper than
HST/NICMOS
 Photometric precision of
+/-2% is reached
 “Second Branch” in CO-K’
may correspond to a much
younger (few 106 yr)
population
 Concentrated very near the
Galactic Center
Circumstellar disks: GG Tau
Dan Potter, U Hawaii (IfA)
 Tidally truncated circumbinary
disk
 Keplerian disk extent ~ 180-260
AU
 resolved imaging polarimetry
of system
 Nature of irregularities?
Performance of Hokupa’a on
Gemini
 Hokupa’a performs best with bright guide stars (V<15) and good
seeing conditions (d < 0.7”)
Delivers image in JHK < 0.1”
 Complements HST observations
 Photometry in crowded environments

 Hokupa’a is a powerful tool

to explore the environment of bright objects, close companions,
circumstellar disks and to study inner regions of galaxies, QSO host
galaxies
Mid-IR Imaging with OSCIR
On Gemini North
 Designed and built by Charlie
Telesco et al. (U of
Florida/NSF and NASA)
 Mid IR (8-25 mm) imager and
low resolution spectrograph
 128x128 Si:As IBC detector
11”x11” on Gemini
 Pixels of 0.089”/pix

The Hot Molecular Core in G29.96-0.02
radio continuum (3.5 cm)
NH3 (4,4)
Crosses:
H2O masers
1”
May represent
intense accretion
phase of high-mass
star formation
Figure from Cesaroni et al. 1998
First Direct Mid-IR Image of a Hot Molecular Core
18.2 mm
F(18 mm)
= 4.6 Jy
De Buizer (CTIO) et al.
L 1448 N(AB)
Class 0 Protostar
(Primary Stellar
Accretion Phase)
Binary Pair
Separated by 7”
IRAS
IRAS
Ciardi et al. (U. Florida)
• A emits all mid-IR
• Extended structure?
• 2-component BB
The Jet of M87 at 10 mm
Eric Perlman et al. (UMBC)
HST/WFPC2
HST/F300W, 0.3 mm
M87 Jet
OSCIR, 10.8 mm
 Deepest image ever taken in the mid IR.
 Sensitivity (1s, 1h): 0.1 mJy on point source; 0.028 mJy/pix
 Nucleus is point-like (FWHM ~ 0.5 arcsec)
 Knots A, B, C show structure; fluxes consistent with non-thermal radio emission
MIR emission in a Starburst
Galaxy SBS 0335-053
S. Plante (U Laval) & Marc Sauvage (CEA)
HST/WFPC2
 Blue Compact Galaxy with
1/40 O/Hsun (gas) at 54.3
Mpc

6 SSCs (<25 Myr)
 Exceptionally bright in at
10um

But not coinciding with HST
knots
Gemini OSCIR N band
Spectral Energy Distribution of SBS0335-052
Flux (mJy)
Q=50.2 mJy ± 30%
Output from Dusty
N=10.3 mJy ± 50%
t = 50
T = 1300 K
30%Sil 40%Grf 30%AmC
Wavelength (mm)
“Dusty” results on SBS
0335-053
 tV ~ 50 mag


21 mag from ISO (Thuan et al. 1999)
0.6 mag from optical spectra (Izotov et al. 1997)
 Young stellar population

>50% of SF undetectable from NIR/visible
 Amorphous carbon (more than silicates – SN),
though no PAH bands detectable from ISO spectrum

Standard MRN distribution (53% Silicates, 47% graphite)
does not reproduce the SED
Performance of OSCIR
on Gemini
 Best achieved point-source sensitivity: 0.1 mJy at 10.8
mm (N band), 1s, 1 hr of chopped integration
 Best achieved angular resolution: 0.3’’ FWHM at 10.8
mm (N band)

approximately diffraction limited
 OSCIR has contributed fundamentally to engineering
of the Gemini Telescopes secondary mirror system


Chopping, nodding, fast-guiding and close-loop focus
Preparation for T-ReCS facility instrument
Status of the Gemini
Telescopes and Instruments
 Call for Proposals for Semester 2002A (1-Feb – 31 July
2002) issued


50% science time on Gemini North, 40% on Gemini South
On-going telescope commissioning
• Examples: tuning closed loop systems, integrating high-level
software, overall systems reliability and maintenance, mirror
silver coating
Gemini Control Philosophy
Control model: “Classical” Open Loop Control
Gemini Control Philosophy
“P1”
S (x, y, z, t)
Control model: Full Active Optics Control
“P2”
Detailed Definition of
Observations…high-z SN
…Resulting NIRI Data
High-z SN (z=1.1)
H ~ 23 mag in ~2 hr
Status of the Gemini
Telescopes and Instruments
 Call for Proposals for Semester 2002A (1-Feb – 31 July
2002) issued


50% science time on Gemini North, 40% on Gemini South
On-going telescope commissioning
Status of the Gemini
Telescopes and Instruments
 Call for Proposals for Semester 2002A (1-Feb – 31 July
2002) issued



50% science time on Gemini North, 40% on Gemini South
On-going telescope commissioning
New and on-going instrument commissioning
 Gemini North instruments
 Hokupa’a/QUIRC
 CIRPASS – near IR IFU
 NIRI*
 GMOS*
*Facility instruments
 Gemini South instruments
 Flamingos – near IR MOS
and imager
 Phoenix – near-IR high res
spectroscope
 Acquisition Camera* –
simple optical imager
 T-ReCS* – mid-IR imager
NIRI Status
 Flexure and other problems caused
cancellation of 2001A use

‘Final’ fix to flexure problem to be tested this
month
 Throughputs and sensitivities has been
measured for imaging and spectroscopic
modes
 Integration with high-level s/w is
underway

Observing Tool (OT) for Phase II definition
was released in May; 2001B release is due
early October
 Data processing scripts under internal
testing

Due for release with first SV data
NIRI Commissioning Results
 JHK imaging of starforming region
AFGL2591


Images have 0.4” FWHM
(closed loop PWFS2)
Data obtained with 7580% ‘shutter-open’
efficiency (under high-level
s/w control)
GMOS Status
 GMOS delivered to
Gemini-N in June
 First commissioning run
was in Aug/Sept

Very successful: tested
imaging, long-slit, MOS and
IFU spectroscopy
GMOS Imaging
3 off 2048x6048
CCDs
r-band image
60s exp
0.58” FWHM
Shadow of
OIWFS
5.5 arcmin FOV
(Abell 383 cluster
at z=0.19)
GMOS Multi-Object
Spectroscopy
Test mask with
20 slits, each
1 arcsec wide
30 x 30min
exposures
GMOS Multi-Object
Spectroscopy
Test mask with
20 slits, each
1 arcsec wide
30 x 30min
exposures
Galaxy with
r~21.5 mag
at z=0.28
GMOS IFU Spectroscopy
2 integral field
units for
‘object’ and
‘sky’
GMOS IFU Spectroscopy
Reconstructed
image of star as
seen by IFU
Raw spectra of extended object (M32):
63000+ spectra taken on first commissioning
night
Commissioning of Gemini South:
Near-IR Test Camera (ABU)
K-band image of GGD27
star-forming region (20s exp)
GMOS multicolour image
of NGC628
(0.55 arcsec)