Transcript Gemini - Sochias

2009 Gemini Highlights
Jean-René Roy
SOCHIAS Annual Meeting - Santiago, Chile, 14-16 January 2009
Since 1993, Gemini:
an international partnership
 Gemini members are:
United States (50%), United Kingdom
(25%), Canada (15%), Australia (5%)
Argentina (2.5%) and Brazil (2.5%)
- Hosts: Chile, Hawaii
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Two 8 m telescopes optimized for
visible/infrared wavelengths
– GN on Mauna Kea (4200 m),
Hawaii
– GS on Cerro Pachon (2700
m), Chile
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Current Gemini International
Agreement ends on 31 Dec. 2012.
Negotiations for post-2012 have
started.
… Gemini : one observatory, two telescopes
Since 2000
Gemini North, Hawaii
Gemini South, Chile
Cerro Pachón 2900 m
Since 2001
Instrument suite at Cass
Gemini South
 Optimized execution of programs
 High completion rate of programs
 High shutter open efficiency
Michelle
GMOS-S
GNIRS
NIRI
T-ReCS
Altair
Gemini North
GMOS-N
Two sites 11,000 km apart +
Gemini archive in Canada
Total staff
~185
CADC-archive
GN = 55%
GS= 45%
~1/3 Eng
~1/3 Sci
~1/3 Admin
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NGOs
Mauna Kea
Cerro Pachon
A brief history of exo-planet
imaging at Gemini
A brief history of exo-planet imaging at Gemini
2001: Two ultracool
companions to the young
star HD130948
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Gravitationally bound pair
Very low mass ultracool objects
– Pair separation = 0.134+/0.002”
– ~7% of the Sun mass
Binary = 1.13 Msun total
– Semi-major axis = 2.4 AU
– period ~ 10 yr
Primary < 1 Gyr
Potter et al. ApJ, 2001
2002: Crossing the BD desert
in 15 Sge
0.06 Msun (48 Mjup) L dwarf companion HR 7672; 14 AU from star
Gemini/Hokupa’a. BD can exist that close to the main star (Liu et al. AJ, 2002)
…but Brown Dwarfs are NOT planets.
Young Jovian planets are 100 – 1000 times fainter
Subaru
Gemini N
Keck
CFHT
The race for imaging the first extrasolar planet is on.
Gemini, Keck, Subaru, VLT or HST?
Slides from 2/17/02
Gemini Deep Planet Survey*
Deepest and Largest Exo-planet Imaging Survey
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NIRI/ALTAIR AO search for giant planets and
brown dwarfs around 86 stars
– 1.6 m 5 sensitivity to  > 0.5”
 m = 9.5 at 0.5”
 m = 12.9 at 1”
– or 2 Mjup for 100 Myr old K0 star at d ~ 22 pc at
40-200 AU separation
Second epoch observations of 48 stars confirm all
candidates as unrelated background stars
95% upper limit of fractions of star with at least one
planet of 0.5 - 13 MJup are
– 0.28 for 10-25 AU
– 0.13 for 25-50 AU
Final ADI
Jovian planets are rare around late- and
Sun-like stars ==> chance of young Jovians to be
in the 10-50 AU zone is max ~20%
Lafrenière et al. 2007, ApJ
Angular differential imaging demo
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“low hanging fruit”: large Jovian
“companion” of IRXS J…
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Gemini North ALTAIR NIRI discovery of 8 MJup
“companion” to K7-type solar mass star (d ~ 150
pc)
– In ~5 Myr-old Upper Scorpio association
– At r = 2.22” or 330 AU orbit?
Spectroscopy of Jovian planet
– L4-type with Teff ~ 1800 K
Needs proper motion measurements over next 23 yrs to establish whether planet is bound to star
of chance superposition.
After 10 years of trials, first imaging
of a self-luminous Jovian planet ‘around’
a normal star, I.e. lowest mass companion
Imaged around normal star so far.
Lafrenière et al. 2008, ApJL
HR 8799: Three More Planets!
HR 8799: ~60
Myr, F-type
C. Marois et al.,
2008, Science
First images of
“planetary
Family”
M~3 to 13 MJup
Planet Luminosity
(Lsun)
Models of Young Planet
Luminosity
5 Myr, 8 MJup planet!
(Lafreniere et al. 2008)
Marley et al. 2006
Age
In 3rd quarter of 2008: a
beautiful crop of exoplanets!
2009+: NICI at Gemini South
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NICI AO performance as good or better than expected at radii less than ~1.4
arcsec
Contrast at larger radii is limited by array controller issues, read noise, and short
exposure times used for these tests (ADI)
Super Gemini Planet Imager at
GS in 2011
Other recent
science accomplishments
BBQ Temperature Brown Dwarf*
• CFBDS0059 found by i’-z’
imaging on CFHT and
spectral characterization by
Gemini (NIRI) and VLT
– Coolest BD with Teff ~ 625
K and log g ~ 4.75
– Evolutionary models
indicate age of 1-5 Gyr
and 15-30 MJup
– CFBDS0059 and ULAS
J0034 could be the first Y0
dwarfs detected
Spectral indices defining T dwarf
saturate below 700 K. New index
of NH3 absorption in the H band
introduced.
Delorme et al. 2008, A&A
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SN2008d: A Unique Opportunity
Soderberg et al. 2008, Nature
3 SN in NGC 2770
over ~10 years
SN 2008d discovered
at the moment of
explosion Jan 10
Rapid Gemini-GMOS
spectroscopy follow-up
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Gemini North-GMOS g’, r’, I’ and H, March 6, 2008
Present at the Birth of SN 2008d
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Birth of SN 2008d (SN Ibc) signaled by
extremely luminous X-ray outburst
– First ever event detected so early
(10 Jan 2008) - Swift
– NGC 2770 at d = 27 Mpc
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Almost daily monitoring with GN/GMOS
from the first day (GN-2007B-DD-9) up
to the end of Jan, and weekly
spectroscopy from Feb. 1st until mid
May 2008
– Clear evolution from featureless
continuum to broad absorption
lines, and finally to deep absorption
features of moderate widths
SN 2008d shows emergence of strong
He I features of He-rich SN Ibc, unlike
GRB-Supernovae.
Soderberg et al. 2008, Nature
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Massive “Dead” Galaxies at z >2
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“Dead” massive galaxies at z > 2
– Previous deep GNIRS
spectroscopy had revealed 45%
of the small sample to have low
or no SF
– New very deep GNIRS spectrum
of one “dead” object at z ~ 2.2
confirms very low SF
• Most massive galaxies
formed early
• And nuclear/black hole
driven winds may act as
“birth control”
High z galaxy research enabled by efficient
and versatile X-dispersed mode of GNIRS
Kriek et al. 2006, 2008, ApJ
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GN LGS AO: Ops highlights
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Successfully (and somewhat painfully) operating
Laser Guide Star Adaptive Optics (LGS-AO) at
Gemini North
– Demand: 200h in queue per semester, leading to
50-60 scheduled nights per semester
– Gaining experience that will help with deployment
of LGS-AO at GS
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Laser AO use requires cloudless sky and
seeing better than ~ 0.8” in the optical
– Occurs ~25% of the time
– Schedule 3.5-4 times as many LGS nights
in queue as approved queue science time
Operating under the Laser Clearing House rules
for clearance to propagate the laser
– Target positions need to be pre-approved
– Each target has clearance only in specific
time intervals
Mix LGS AO programs with non-LGS queue to
make optimal use of telescope time
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Deep into the
core of
NGC 4244
with
Gemini North
NIFS
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A Rotating Nuclear Stellar Cluster
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ALTAIR/NIFS LGS AO spectroscopy
of flattened nuclear star cluster in
edge-on spiral NGC 4244
– Multiple components
– Strong rotation +/-30 km/s within
the central 10 pc
• Both young disk and
spheroidal components rotate
• Rotation is in same direction
as normal disk
• 1.7 x 106 solar mass located
< 8 pc from core
Primary formation of NSC through episodic
accretion of material from the disk, gas or
young star clusters.
Seth et al. 2008, ApJ
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2009: Current deployment of
instruments on GN & GS
Mauna Kea
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GMOS
ALTAIR+LGS*
NIRI*
MICHELLE
NIFS*
GNIRS*
GLAO*
WFMOS
Cerro Pachón
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GMOS
T-ReCS
Phoenix
NICI*
FLAMINGOS-2*
MCAO/Canopus*
GSAOI*
GPI*
*AO instrumentation
FLAMINGOS-2: Near IR
MOS for Gemini South
1-2.5 mm
FOV 6’x6’
for imaging
FOV 2’x6’
for MOS
We “hope”
To deploy
F-2 in 2009A
GLAO MK Modeling Results
Improvements in
FWHM are
consistent, about 0.2
arcsec at H
Ensquared energy
improvements
between 50% and
100% in 0.2 arcsec
Current 20percentile
IQ would be achieve
80% of the time.
Summary
Coming very soon:
• GNIRS “reborn”
– recommissioning 2009A
• NICI
– Planet survey has started
– Available for all type of
science, not only planet
search
• FLAMINGOS-2
– Acceptance tests being
analyzed
• GMOS-N CCD replacement
in 2009; GMOS-S to follow
New development:
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GPI
– In construction; completion in
2011
WFMOS
– designs studies under way;
end date Feb. 2009
– Gemini negotiation with
Subaru on-going
GLAO
– Site survey data imply
excellent GLAO performance
on MK
Na Kilo Hoku o Mauna Kea