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

30’

(7 k

pc)

20”

(80

pc)

M33

M33 Core Optical-IR CMD

Luminosity Function

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

First Direct Mid-IR Image of a Hot Molecular Core

18.2 m

De Buizer (CTIO) et al.

F(18 m) = 4.6 Jy

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

The Jet of M87 at 10 mEric Perlman et al. (UMBC)

HST/WFPC2

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

Control model: “Classical” Open Loop Control

Gemini Control Philosophy

Control model: Full Active Optics Control

(x, y, z, t)

“P2”“P1”

Gemini Control Philosophy

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

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

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

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 multi-colour

image of NGC628

(0.55

arcsec)