the circumgalactic medium, the intergalactic medium,...
TRANSCRIPT
The Circumgalactic Medium, the Intergalactic Medium, and Prospects
with TMT
Taotao Fang ⽅方陶陶
Xiamen University 厦⻔门⼤大学
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2014.11 Beijing
• The circumgalactic medium (CGM) and the intergalactic medium (IGM) – Introduction, discoveries in the nearby universe, some of our own work !
• What can TMT/MOBIE do? – Revolutionize the CGM/IGM study at high z universe !
• China’s involvement in TMT/MOBIE
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A Very Success Story of Cosmic Structure Formation and Evolution
Vogelsberger et al. (2014)
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“The fraction of baryons detected in all forms deviates monotonically from the cosmic baryon fraction as a function of mass.” McGaugh et al. (2009) What is sustaining the star formation in
galaxy if only 1 to 2 Gyr of gas is present?
What cause the biomodality in galaxies?
The mismatch between the galaxy LF and DM halo mass distribution?
However, when it comes to galaxy formation and evolution …
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Accretion/Inflow
Feedback/Outflow
Circumgalactic Medium (CGM)
Recycling
IGM IGM
IGM
IGM
ISM
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•High-ionization ions ➡ OVI, CIV ➡ 10^5 < T < 10^6 K ➡ Warm CGM
•Low-ionization ions ➡ SiII, MgII … ➡ T < 10^4-10^5 K ➡ Cool CGM
•H, He-like ions ➡ OVII, OVIII, NeIX ➡ T > 10^6 K ➡ Hot CGM
Some Highlights of the CGM Study in the Nearby Universe
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HST/Cosmic Origin Spectrograph (Ultraviolet)
Chandra and XMM-Newton (X-ray)
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Tripp et al. (2002)
Long-standing puzzle in quasar absorption line study: Where are these absorbers? Galaxies or the IGM?
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•39 QSOs at redshift around 0.5 !
•44 foreground galaxies with R < 150 kpc, with z between 0.15 and 0.35 !
• 28 star-forming galaxies, 16 passive galaxies
COS-Halos Survey
Tumlinson et al. (2013)
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Absorbers are associated with galaxies!
Tumlinson+ 2012
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Absorbers are associated with galaxies!
Tumlinson+ 2012
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Absorbers are associated with galaxies!
Tumlinson+ 2012
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Absorbers are associated with galaxies!
Tumlinson+ 2012
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Absorbers are associated with galaxies!
Tumlinson+ 2012
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Absorbers are associated with galaxies!
Tumlinson+ 2012
And highly ionized OVI are associated with star-forming galaxies!
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Tumlinson+ (2011)
Confirming our prediction …
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In the Milky WayObservation:
Expectation:
Another puzzle: Where are the missing galactic baryons?
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Werk+ 2014
•COS-halos survey !
•A substantial amount of cool CGM (cold gas), comparable to the galaxy stellar mass! !
• A negligible amount of hot X-ray CGM (which we disagree!!!)
A surprising discovery from the absorption line study!!!
Fang+ 2003
Detection of z=0 OVII Implying the absorber is local, and hot! T ~ 1-2 million degree!
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XMM-Newton Survey of Extragalactic Targets
Fang+ 2014
• 43 extragalactic sources, 13.5 million seconds
• 12 BL Lacs, 31 Seyfert 1 galaxies
• Column density • Sky covering fraction:
uniform distribution • There may exist a
significant amount of hot CGM!
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The Intergalactic Medium and the “Missing Baryons” Problem
23% DARK MATTER
73% DARK ENERGY
4% BARYONS
4% BARYONS
•Big bang nucleosynthesis !
•Cosmic microwave background !
•High z Ly-alpha forest
Three independent measurements gave a very consistent result of baryon fraction!
However, in the local universe:
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Galaxy: star, atomic & molecule gas
Galaxy cluster: intracluster medium
cold gas in the intergalactic medium
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TOTAL: ~ 2%e.g., Fukugita et al. (1998)
Recipe: cosmological model gravity gas dynamics !
Prediction: most missing baryons reside in these filaments! !
Warm-Hot Intergalactic Medium the missing baryons: (1) in the IGM; (2) warm-hot (105 < T < 107 K); (3) moderate overdensity (5 - 200)
Numerical Modeling
Cen & Ostriker (1999); Dave et al. (2001); ...
Vogelsberger et al. (2014)
Using Blazar Absorption Line to Probe the Missing Baryons
Best tracers •OVII, in X-ray •Broad HI, in UV
Best background source: •Blazar (featureless)
H2356-309 Campaign: Searching for the Missing Baryons
Sculptor Wall Superstructure Filamentary structures
in numerical simulations correspond to local galaxy superstructures
H2356-309 Campaign: Searching for the Missing Baryons
H 2356-309
Sculptor Wall Superstructure
Intersection at z = 0.03
Between 2010 and 2014, we were awarded with the following telescope time: • 500 ksec with Chandra • 600 ksec with XMM-Newton
• 7-orbit with HST/COS
Chandra
XMM
Sculptor Wall WHIM absorber @ z = 0.03 The First Clear Detection of the Missing baryons
in X-ray Absorption
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Next Steps?• XMM RGS large project (500 ksec)
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Next Steps?• XMM RGS large project (500 ksec) • Targeted search along other sightlines
Ren & Fang (2014)
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Next Steps?• XMM RGS large project (500 ksec) • Targeted search along other sightlines • Can we use HI as the tracer? (HST, 7-orbit)
HI Lyα (BLA) Richter et al. (2006)
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HST/Cosmic Origin Spectrograph Observation of H 2356-309
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z = 0.03
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z = 0.03
z = 0.06
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z = 0.03
z = 0.06
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•A single narrow component cannot provide an adequate fit to the HI line profile (right panel)
•A broad line on top of a narrow component improves the fit significantly (left panel)
•This broad component, if confirmed, implies an absorber temperature consistent with the measurement from X-ray
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What Can TMT/MOBIE Do in Studying the CGM/IGM?
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Some Science Goals of TMT/MOBIE• Stellar evolution and white dwarfs • Metal poor stars • Resolved Stellar Populations in the Local Group • The Dark Matter Distribution in Nearby Elliptical Galaxies • 3D Baryonic Structure During the Epoch of Galaxy
Formation • The Stellar and Gaseous Content of L_star Galaxies at z =
2 − 5 • QSO Pairs: Revealing AGN and Massive Galaxy
Formation at z > 2 • Transients
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Probe the CGM in this crucial region!
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TMT Survey of Baryonic Structure
Survey Sky Area #Targets Exp Total
Galaxies: z = 1.6 - 3.5
4 x (2 x 0.56) sq deg
120,000 @ AB < 26.5
1 hour for SNR > 5 @ R = 500
1000 hours
IGM z = 1.6 - 3.5
4 x (2 x 0.56) sq deg
15,000 @ AB < 24
4.5 hours for SNR > 35 @ R = 5000
450 hours
• Survey both galaxies and the IGM over a volume of the z = 1.6 – 3.5 universe that is as statistically representative as the Sloan Digital Sky Survey (SDSS) redshift survey at z ~ 0.1
•Surface density of IGM probes to R=24 is 5000/sq deg •Volume covered would be 10^8 Mpc^-3(co-moving) in 4.5 sq. deg.
TMT:Wide Field Telescope @ High z!
TMT/MOBIE and China’s Involvement
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Wide Field Optical Spectrograph
(MOBIE)
TMT/MOBIE !
M1- M2 - M3 - Sci. Instruments
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Multi-Object Broadband Imaging Echellette (MOBIE)
(Bernstein 2013)
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AGWFS ADC
(Bernstein 2013)
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Design Requirements
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MOBIE Important Timeline• Feasibility study phase: June 2008 - Dec 2008
– Optical design and fabrication study • Conceptual design phase:
– Phase I: June 2009 - Dec 2010. Initial conceptual designs, cost estimates for TMT
– Value Engineering Study: Jan 2011 - Feb 2013. De-scope options and recommendations
– Phase II: March 2013 - Oct 2013. Continue conceptual designs, integrate MOBIE project with TMT project management control system and integrated project schedule
– Mini-study: April 2014 - Feb 2015 – Phase III: Jan 2015 - Dec 2015. Complete outstanding CDP
work and hold the conceptual design review • Preliminary design phase: March 2016 -
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Planning: MOBIE & IRMS
!u Dec. 16-21, Shanghai, Nanjing, Beijing u TMT: Bhatia, Simard, Roberts, Ellerbroek, Konidaris, Radovan (video) u University of Florida: Prof. Jian Ge u China: 40 participants from 16 institutes and universities
China-TMT Instrumentation Planning Workshop
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MOBIE Stakeholder Meeting Beijing, April, 2014
• ~ 60 participants from China, United Sates, Japan, India, Canada"
• Go over the committee report from the October 2013 Conceptual Design Handover Workshop "
• … and mini-study state of work: 12 mini-studies, involving 12 subsystems"
• China is participating in 10 mini-studies, including 6 mini-studies as managing institutes (see next page)"
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MOBIE Stakeholder Meeting Beijing, April, 2014
TMT.INS.MGT.14.039.DRF04!
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MOBIE Mini-Studies
• 4/24-4/29 Sandra Faber, Luc Simard, and Matthew Radovan visited CIOMP, NIAOT, USTC, and SIOM (along with Taotao Fang and Zhixia Shen from CTMT)"
• May - present: regular telecom to discuss the progress of each mini-study ""• Discussion with each team: Mini-study milestones, associated deliverables and tasks required to complete the deliverables"
• Mini-studies run through Dec 2014, with a review in Jan 2015"
Summary
• The material in the interface between galaxies and the IGM, the CGM, plays a key role in regulating galaxy formation and evolution, as demonstrated by UV/X-ray observations of nearby galaxies
• TMT/MOBIE will revolutionize this field by studying the CGM and the IGM at redshift 1.5 to 4, where both star formation and quasar activities are at their peaks
• China actively involves in the design of MOBIE; Our technology is mature and ready; but we need significant involvement in developing science cases for MOBIE (as well as other first-light instruments)!!!
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