Early Science Results and Status of the Gemini Telescopes Prepared by Phil Puxley Barolo, October...
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Transcript of Early Science Results and Status of the Gemini Telescopes Prepared by Phil Puxley Barolo, October...
Early Science Results and Status
of the Gemini Telescopes Prepared by Phil Puxley
Barolo, October 2001
Gemini North, Hawaii - 4200 mBeginning of science operations: 2000B
Gemini South, Chile - 2900 mBeginning of science operations: 2001B
Gemini North: Early science with “visitor”
instrumentsWhy? 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
M32
K’-band20”x20”
FWHM=0.12”
Bright *AGB tipK = 15.5
Davidge et al. 2000, ApJ, 545, L89 = FIRST PAPER
Engineeringinto science
Small H-K color dispersion - Brightest stars well mixed throughout - No evidence for radial age gradient
The Stellar Content of the Central Regions of
M33
A.W. Stephens & J.A. FrogelA.W. Stephens & J.A. FrogelThe Ohio State UniversityThe Ohio State University
First results on center of M33
Complicated CMDRange of stellar agesLF slope steeper than bulge of our GalaxyDisk-like stellar distribution to ~3”No significant radial variations in LF or CMD
QSO “absorbing” galaxiesMark 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(5 ) ~ 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/QUIRCDEMONSTRATION 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
Program Support/DRTim Davidge, HIABob Blum, CTIO
Angela Cotera, Steward Obs.Mark Chun, Gemini
Instrument SpecialistsMark Chun, GeminiJoe Jensen, Gemini
Wolgang Brandner, UH-IfADan Potter, UH-IfA
CoordinationF.Rigaut
Science definitionVicky Alonso, Cordoba
Robert Blum, CTIOMichael Burton, UNSW
Simon Casassus, U.ChileAngela Cotera, Steward
Tim Davidge, HIATom Geballe, GeminiAndrea Ghez, UCLA
Fluvio Melia, StewardDante Minniti, U.Catolica
Mark Morris, UCLAA. Quirrenbach, UCSDDoug Simons, Gemini
Galactic CenterDemo Science
Eleven 20’’x20’’fields
Orange symbol isthe guide star for Hokupa’a.
Field 11 is theArches Cluster
UH-88”, Courtesy W.Brandner, 0.65” seeing
Filters:
•H•K’ •CO•CO cont.
4’
IRS7 SgrA*
>10 stars per arcsec2 at K~18
Bow shock
Very high extinction clouds
40”
5”
>220 stars in 5”x5”
IRS8 (bow shock)
Gemini N/Hokupa’a-Quirc (U of H/NSF)
Analysis of GC DataFrancois 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 m) 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
Figure from Cesaroni et al. 1998
radio continuum (3.5 cm)
1”
NH3 (4,4)
Crosses:H2O masers
May represent intense accretion phase of high-massstar formation
L 1448 N(AB) Class 0 Protostar(Primary Stellar Accretion Phase)
Binary Pair Separated by 7”
Ciardi et al. (U. Florida)
• A emits all mid-IR• Extended structure?• 2-component BB
IRAS
IRAS
OSCIR, 10.8 m
HST/F300W, 0.3 m
Deepest image ever taken in the mid IR. Sensitivity (1, 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
M87 Jet
MIR emission in a Starburst Galaxy SBS 0335-053
S. Plante (U Laval) & Marc Sauvage (CEA)
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
HST/WFPC2
Gemini OSCIR N band
Flu
x (m
Jy)
N=10.3 mJy ± 50%
Q=50.2 mJy ± 30%
Wavelength (m)
= 50T = 1300 K30%Sil 40%Grf 30%AmC
Output from Dusty
Spectral Energy Distribution of SBS0335-052
“Dusty” results on SBS 0335-053
V ~ 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 m (N band), 1, 1 hr of chopped integration
Best achieved angular resolution: 0.3’’ FWHM at 10.8 m (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
InstrumentsCall 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
Status of the Gemini Telescopes and
InstrumentsCall 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
InstrumentsCall 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 instrumentsHokupa’a/QUIRCCIRPASS – near IR IFUNIRI*GMOS*
Gemini South instrumentsFlamingos – near IR
MOS and imagerPhoenix – near-IR high
res spectroscopeAcquisition Camera* –
simple optical imagerT-ReCS* – mid-IR
imager
*Facility instruments
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 star-forming region AFGL2591 Images have 0.4”
FWHM (closed loop PWFS2)
Data obtained with 75-80% ‘shutter-open’ efficiency (under high-level s/w control)
GMOS StatusGMOS delivered to
Gemini-N in JuneFirst commissioning
run was in Aug/Sept Very successful: tested
imaging, long-slit, MOS and IFU spectroscopy
GMOS Imaging
Shadow of OIWFS
5.5 arcmin FOV
3 off 2048x6048 CCDs
(Abell 383 cluster at z=0.19)
r-band image60s exp 0.58” FWHM
GMOS Multi-Object Spectroscopy
Test mask with20 slits, each 1 arcsec wide
30 x 30minexposures
Galaxy with r~21.5 magat z=0.28
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)