Selecting the best targets for JWST My personal journey as a MIRI team scientist Margaret Meixner STScI JHU March 7 2013 Hubble Science Briefing Hubble Science Briefing Margaret Meixner ID: 461834
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7 March 2013
Selecting the best targets for JWST: My personal journey as a MIRI team scientist
Margaret Meixner (STScI, JHU)March 7, 2013
Hubble Science Briefing
Hubble Science Briefing - Margaret MeixnerSlide2
Outline of Talk
My personal story as a JWST/MIRI science team memberAstronomers prepare now to use the power of JWST(James Webb Space Telescope)Spitzer and Herschel space observatories find thousands of forming stars in the Magellanic Clouds
Large Magellanic Cloud (LMC)Small Magellanic Cloud (SMC)
My JWST programs on star formation in the Magellanic CloudsHow JWST will discover more forming stars in nearby, but more distant galaxies
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Hubble Science Briefing – Margaret Meixner
7 March 2013Slide3
Margaret Meixner:
Member of the JWST/MIRI Science
Team
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Hubble Science Briefing – Margaret Meixner
7 March 2013Slide4
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JWST Sensitivity:
-typically detects at an order of magnitude fainter than recent and current observatories
-lower is better!
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide5
JWST Sensitivity
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JWST launches in
2018;
appropriate target lists must be developed now…
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide6
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James Webb Space Telescope (JWST)
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide7
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James Webb Space Telescope (JWST)
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide8
Integrated
Science
Instrument Module
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James Webb Space Telescope (JWST)
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide9
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Integrated Science Instrument Module (ISIM)
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide10
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Integrated Science Instrument
Module (
ISIM)
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide11
NIRSpec
NIRCam
NIRISS
MIRI
James Webb Space Telescope: Webb ~2018
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7 March 2013Slide12
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The Mid-InfraRed Instrument
(MIRI)
Hubble Science Briefing – Margaret Meixner
7 March 2013
spectrograph
ImagerSlide13
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MIRI detector
Hubble Science Briefing – Margaret Meixner
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MIRI Arrives at Goddard
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide15
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MIRI Inspected at Goddard
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide16
MIRI Team
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Hubble Science Briefing – Margaret Meixner
7 March 2013Slide17
Why the Magellanic Clouds?
They act as a good astrophysical laboratory:They are nearby: ~50 kpc (LMC) and ~60 kpc (SMC) [the Andromeda Galaxy is about 16 times farther away]Mean metallicity (Z)* is similar to metallicity of the interstellar medium during Universe
’s peak star formation epoch (z**~1.5)LMC: Z~0.5 x Z
SMC: Z~0.2 x Z
Known tidal interactions between LMC and SMC, possibly the Milky WayLong History of Studies & used as a proving ground: Ideal Case study for galaxy evolution
*
metallicity (Z) = percent of elements other than hydrogen and helium
**z =
redshift
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Hubble Science Briefing – Margaret Meixner
7 March 2013Slide18
LMC, SAGE- MIPS: 70
m
Meixner et al. 2006
http://sage.stsci.edu/
SAGE
team
Meixner
et al. 2006
IRAC 3.6
m: old (evolved) stellar populations
IRAC 8.0
m: dust emission from ISM
MIPS 24
m: new massive star formation
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Spitzer Survey of the Large Magellanic Cloud (LMC):
Surveying the Agents of Galaxy
Evolution (SAGE)
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide19
7 March 2013JWST briefing - Margaret Meixner
Spitzer wavelengths detect dust, stars & gas
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http://www.spitzer.caltech.edu/images/2627-sig07-011-The-Spitzer-Space-Telescope-SpectrumSlide20
SPIRE 250
mPACS 160
m
PACS 100
m
HERITAGE Team
;
Meixner et al.
submitted
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Hubble Science Briefing – Margaret Meixner
7 March 2013
LMC:
Herschel Inventory of The Agents of Galaxy Evolution (HERITAGE)Slide21
http://sage.stsci.edu
/SAGE SMC team
Gordon et al. 2011
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old (evolved) stellar populations
new massive star formation
dust emission from ISM
SAGE-SMC: Spitzer IRAC & MIPS Imaging of
Small Magellanic Cloud (SMC)
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide22
SPIRE 250
mPACS 160
m
PACS 100
m
HERITAGE
Team;
Meixner et al.
submitted
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SMC
:
Herschel HERITAGE
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide23
Goal of Spitzer and Herschel surveys:
to study lifecycle of baryonic matter using infrared and submillimeter emission from dust. Why is studying dust important? Dust is present at the key transition points of this life
cycle It is present in the ISM (which is the origin of the cycle)
Dust enshrouds the young stellar objects as they form
Dust is produced in the stellar winds of dying stars and in the explosive
supernovae
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Why is studying dust important?
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide24
credit:
http://hea-www.cfa.harvard.edu/CHAMP/EDUCATION/PUBLIC/ICONS/
Intermediate mass stars
High mass stars
Tracing the Lifecycle of Baryonic
Matter
:
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Hubble Science Briefing – Margaret Meixner
7 March 2013Slide25
credit:
http://hea-www.cfa.harvard.edu/CHAMP/EDUCATION/PUBLIC/ICONS/
Intermediate mass stars
High mass stars
Tracing the Lifecycle of Baryonic Matter
:
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YSOs
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide26
Young Stellar Object Evolutionary Stages
Herschel
Spitzer
Hubble & JWST
Young
Protostar
:
Main Accretion Phase
Evolved Accreting
Protostar
Thick disk, accreting,
Herbig
Ae
/Be
Thin disk,
T-
Tauri
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Hubble & JWST
time
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide27
N 66
NGC 602
NGC 346
8.0
m
m
7 March 2013
JWST briefing - Margaret Meixner
~1100 YSO candidates; ~900 new
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Spitzer
Discovers One Thousand Young Stellar Objects in the SMC
Sewilo et al.
submitted
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide28
SAGE IRAC 8
mm
Spitzer:
~1000 YSO candidates Whitney,
Sewilo et al. (2008)~1200 YSO candidates
Gruendl
& Chu (2009)
Pre-
Spitzer
:
~20 protostars known
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Spitzer
Discovers Two Thousand Young Stellar Objects in the LMC
~1800 unique
sources
Star Formation Rate:
~0.1
M
/
yr
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide29
Pre-
Spitzer:~20 protostars known29
SAGE IRAC 8
m
m
Spitzer
Discovers Two Thousand Young Stellar Objects in the LMC
Spitzer
:
~1000 YSO candidates
Whitney
,
Sewilo et
al. (2008)
~1200 YSO candidates
Gruendl
& Chu (2009)
~1800 unique
sources
Star Formation Rate:
~0.1
M
/
yr
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide30
Carlson et al.
2012
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Detailed study by Spitzer finds low-mass YSOs(circles)Slide31
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Carlson et
al. 2012
Detailed study by Herschel finds YSO candidates (red squares)
JWST simulation region (next slide)Slide32
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JWST imaging tiles on N113 star formation region
Seale & Meixner
JWST will detect solar-like stars with
planet forming disks in the LMC!
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide33
NGC 602
But it would be useful to get HST data of a field first,
as we have for an SMC source
SAGE SMC team
Gordon et al. 2011
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Hubble Science Briefing – Margaret Meixner
7 March 2013Slide34
7 March 2013
JWST briefing - Margaret Meixner
MIPS 24µm
IRAC 8.0µm
IRAC 3.6µm, 4.5µm, 5.8µm
Blue= HST Optical
Circles= YSOs
Unclassified
Stage I
Stage I/II
Stage II
Carlson, et al. 2010
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Spitzer & HST image of NGC 602
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Hubble Science Briefing – Margaret MeixnerSlide35
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HST image of NGC 602
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Hubble Science Briefing – Margaret Meixner
7 March 2013Slide36
JWST will
acquire simultaneous
spectral and spatial information
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Hubble Science Briefing – Margaret Meixner
7 March 2013Slide37
Seale, Sewilo, Meixner
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JWST NIRSpec & MIRI
Spectroscopy of selected YSOsExample:
N113, a massive young stellar object
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide38
Seale et al. 2009
MIRI
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LMC N113: Spitzer spectrum reveals a hot massive star
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide39
JWST:
NIRSpec & MIRI
IFU spectroscopyreveals the environmental composition of forming stars
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ISO SWS spectrum
Whittet et al. 1996
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide40
JWST can measure a spectrum of any source detected with Spitzer
In the LMC, we detected 6 million sourcesWith Spitzer we measured spectra of only 2000The faintest sources were unreachable with SpitzerIn the time of 10 seconds to 2 hours, we can measure a spectrum of any source.
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Hubble Science Briefing – Margaret Meixner
7 March 2013Slide41
Pursuing SAGE-like studies
in nearby Galaxies41
With Spitzer, we imaged the Magellanic Clouds with one minute per pointing.
With JWST MIRI, we can detect the same types of forming stars in galaxies as far away as 1 Mpc in one minute per pointing.
The best galaxies should be well studied by Herschel and Spitzer.
the ISM should be mapped in atomic and molecular gas
t
he
stars should be measured and their past well understood
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide42
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M31:
angular size of galaxy: 190’x60’
Hubble Science Briefing – Margaret Meixner
7 March 2013Slide43
M31:
190’ x 2’ strip: total time is ~80 hrs
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Hubble Science Briefing – Margaret Meixner
7 March 2013Slide44
M33:
0.889 Mpc, 71’x42’
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Hubble Science Briefing – Margaret Meixner
7 March 2013Slide45
NGC 6822:
0.490 Mpc, 16’x14’
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Hubble Science Briefing – Margaret Meixner
7 March 2013Slide46
Summary
of TalkPreparing appropriate target lists for JWST, to launch in 2018
Spitzer and Herschel space observatories discovered thousands of forming stars in the Magellanic Clouds
Hubble has surveyed some fields; need more to prepare for JWST
With JWST I will learn about the nature of the material in forming stars in the Magellanic Clouds:
Do they contain a similar amount of water and organic materials?
Do the solar mass stars have enough circumstellar dust
to form planets?
With JWST, I will discover more forming stars in nearby, but more distant galaxies, like M31, M33 and NGC 6822
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Hubble Science Briefing – Margaret Meixner
7
March
2013