# Presentation: 750338

## NASA's 

**Ann Hornschemeier **
**Deputy Project Scientist Constellation-X**
**NASA GSFC**

**Project Scientist:**
**Nick White (GSFC)**
**Facility Science Team Chair:**
**Harvey Tananbaum (SAO)**
**http://constellation.gsfc.nasa.gov**

** ****Studying Dark Energy, Black Holes and Cosmic Feedback at X-ray Wavelengths:  **
**NASA's **
**Constellation-X Mission**

**Con-X Science Booklet: **
**Released Summer 2005**

## Outline

**Constellation-X Mission **
**Dark Energy Constraints using Galaxy Clusters**
**Black Holes & Strong Gravity**
**Cosmic Feedback in the X-ray Band**

## The Beyond Einstein Program

- WMAP

- LIGO

- Hubble

- Chandra

- GLAST

**Science and Technology Precursors**

## The Constellation-X Mission

**25-100 times sensitivity gain over Chandra**
**Baseline of four space-craft working as a single large telescope**

**Black Holes:**** **
**Dark Matter and Dark Energy**
**Cosmic Feedback**
**Life Cycles of Matter and Energy**

**Constellation-X given strong endorsement by US National Academy of Sciences McKee-Taylor & Turner Committee Reports**

## X-ray Mission Collecting Areas

**Suzaku**

## Resolving Power:Collecting Area vs. Spectral Resolution 

## High Spectral Resolution       in the X-ray Band

## Notes on X-ray Spectroscopy

- X-ray spectroscopic workhorse: the He-like triplet  density and temperature diagnostics
- This guides our spectral resolution requirements for hot X-ray plasmas:
- Thermal broadening limits resolution to R~410
***Practical maximum for X-ray plasmas is R~10,000***

**Procyon XMM RGS spectrum (Ness et al. 2001)**

**Notes:**
“Extra” line in the NVI plot is CVI

## Notes on X-ray Spectroscopy

- Absorption spectra of cool plasmas, however, contain complex velocity structures
**Example: NGC 3783, nearby Seyfert 1 (900 ks Chandra HETG; Kaspi et al. 2002) **
**RED: H-like lines**
**BLUE: He-like lines**
**GREEN: Other ions, e.g.,  lower ionization-metals Fe XVII and Fe XXIV****    **
**Constellation-X, with its large effective area, will collect a spectrum of similar quality in 50-100 ks**

## Constellation-X Science

## Constellation-X Science

**Black Holes**

**Cosmic Feedback**

- Life Cycles of Matter

**Dark Energy & Matter**

***What is the detailed structure***
***of the inner accretion disk?***
***How prevalent are ***
***intermediate-mass black holes?***

***Does dark energy  ***
*** ******evolve with redshift?***

***How have accretion disks in ***
***AGN affected galaxy evolution?***
***How do starburst galaxies ***
***enrich the IGM?***

***What is the nature of matter that makes neutron stars?***
***How do stellar outflows affect planet formation?***

## Galaxy Clusters:Constraints on Dark Energy(thanks to Steve Allen, Stanford)

## Cosmology with galaxy clusters

- Galaxy clusters, like supernovae, have a measured property that can be used for distance-*z* comparisons **(f****gas**** measurements; ****e.g., Allen et al. 2002, 2004)**
- Also, number density, spatial clustering and evolution of clusters are all strong functions of dark energy **(Cluster luminosity/mass function measurements; ****e.g., Majumdar & Mohr 2003)**

***Both require large samples (>> hundreds) of large, dynamically relaxed clusters where hydrostatic equilibrium holds (identified in e.g., the ROSAT All Sky Survey)***

## X-ray Emission from Clusters of Galaxies

- X-ray emitting gas dominates                                          the overall baryonic mass in                                  clusters (*M*gas~ 6*M*stars;                                                  e.g., Fukugita, Hogan & Peebles 1998).
**Observables:****    **
**X-ray surface brightness                                        profile.**
**Deprojected (spectrally-determined) temperature (*****kT) *****profile**
**+ assumption of hydrostatic equilibrium  ****                         ****	****	****	****→**** *****M(r)***

**Chandra image of MACS1423+24 (z=0.54)**

**Notes:**
Hydrostatic Equilibrium:
M(<r) T(<r)3/2
Bremsstrahlung:
L(<r)  T(<r)2 

## fgas Measurements withClusters of Galaxies

- Galaxy clusters are so large that their matter content should provide a fair sample of matter content of Universe.

- mass

- cluster

- total

- mass

- gas

- ray

- -

- X

- f

- gas

- 

-  If we define:

- gas

- 0.5

- gal

- f

- 0.19h

- f

- 

- )

- 0.19h

- (1

- f

- f

- f

- f

- 0.5

- gas

- gas

- gal

- baryon

- 

- 

- 

- 

- )

- 0.19h

- (1

- f

- f

- 0.5

- gas

- b

- baryon

- b

- m

- 

- 

- 

- 

- 

- 

*b*

*b*

- Then:

**Since clusters provide ~ fair sample of Universe**** ****f****baryon****=b****Ω****b****/****Ω****m**

## fgas Dependence on Distance(Allen et al 2005, Rapetti et al. 2005)

**The measured fgas values depend on the distance to the clusters as f****gas**** ******** d****A**** ****1.5**** **
**Distance dependence arises from geometry and assumption of hydrostatic equilibrium**

-     **SCDM ****(****Ω****m****=1.0, Ω****Λ****=0.0****) ****                                                   ****Λ****CDM (****Ω****m****=0.3****, ****Ω****Λ****=0.7****)**

## Cosmological Parameters(Allen et al. 2005 DETF Paper)

- Con-X’s effective area critical to study large sample of clusters
- Expect a large snapshot survey followed by deeper spectroscopic observations of relaxed clusters
- will achieve fgas measurements to better than 5% for individual clusters:
**Corresponds to ********M****=0.300********0.007,         ************=0.700********0.047**
**For flat evolving DE model,               *****w*****0**** = -1.00********0.15, *****w*****'**** = 0.00********0.27**

**Clusters**

**SNIa**

**CMB**

***Constraints are similar &***
*** ******complementary to SN Ia studies***

## Black Holes:Strong Gravity and the Inner Accretion Disk

## Fe K:  Accretion Disk Structure

**XMM-Newton obs. of Mrk 766**
**Credit: Turner et al. (2005; astro-ph/0506223)**

- Fe K fluorescence from surface layers of thin, Keplerian accretion disk
- Chandra/XMM  beginning to probe structure on orbital/sub-orbital timescales in outskirts of accretion disk
**Con-X will do the same for ~100-200 nearby AGN**

**Energy (keV)**

## Beyond Einstein:Probing Strong Gravity with Constellation-X

- The Iron fluorescence emission line is created when X-rays scatter and are absorbed in dense matter, close to the event horizon of the black hole.
- Test of General Relativity in the strong field regime

- Theoretical ‘image’ of an accretion disk.

**ASCA X-ray spectrum**
**of MCG-6-30-15**
**Tanaka et al. 1995**

## Inner Accretion Disks: MCG-6-30-15  

- MCG-6-30-15 (d=37 Mpc)
- MBH ~ 106 – 2****107 M
- Strong time variability of line profile:  emission at <6 gravitational radii
- Relatively common in ASCA studies of Seyferts (14/18 have resolved Fe K lines; Nandra et al. 1997)
- Typically line energy ~6.4 keV and =0.43± 0.12 keV

**ASCA X-ray spectrum**
**of MCG-6-30-15**
**Tanaka et al. 1995**

**Notes:**
Many of the lines observed were asymmetric indicating gravitational redshift.
The velocity width of 0.43 keV corresponds to approximately 50,000 km/s
Peak energy of 6.4 keV indicates fluorescence from near-neutral material, but difference in energy
from neutral Fe up to FeXVII is less than 20 eV  

## Constellation-X’s Role:Reverberation Mapping 

- Current limitation:  vast range of black hole angular momentum fits same Fe K data (e.g., Dovciak, Karas & Yaqoob 2004)
- Con-X will track X-ray flares across accretion disks via reverberation effects, constraining the nature of space-time around black holes (Young & Reynolds 2000)

**3               5              6               9**
**                      ****Energy (keV)**

**Constellation-X simulation of**
**a nearby Seyfert galaxy**

## Black Holes: Structure of the Inner Accretion Disk

**Armitage & Reynolds (2003)**

- Tracking material around accretion disks with X-ray spectroscopy
- allows us to probe the nature of space-time very near the black hole

**Notes:**
The most powerful technique for studying the inner accretion disk is the broad iron flurescence line seen in X-ray spectrum of many accreting black holes (e.g., Tanaka et al. 1995; Reynolds & Nowak 2003).  The line is emitted by the surface layers

## Cosmic Feedback

## Definition of Feedback

- Definition of feedback:
***Return, ******via outflows******, of mechanical energy, radiation, and chemical elements from star formation and black holes to the interstellar and intergalactic medium***
- Self-regulation of processes across vast scales (e.g., correlation between stellar bulge mass, velocity dispersion and nuclear black hole mass in galaxies: Magorrian relation)

## AGN Feedback

- Large scale-structure simulations require AGN feedback to regulate the growth of massive galaxies (e.g., Di Matteo et al. 2005, Croton et al. 2005 )
- Non-dispersive X-ray spectroscopy of clusters needed to probe hot plasma (Begelman et al. 2003,2005)
- Powerful AGN outflows in the Universe at* z*=1-3  Chandra/XMM have studied highly ionized outflows in *local* AGN (NGC 3783; Kaspi et al. 2002)

**Con-X simulation **
**of BAL QSO    **
**(S.Gallagher, UCLA)**

- Perseus Cluster
- of Galaxies
- (Chandra image)

**Notes:**
Only X-rays can probe all the outflow material, from cool dust to highly ionized gas

## Supernova (Stellar) feedback Wind plasma diagnostics (D. Strickland, JHU)

**M82 Chandra central 5x5 kpc**
**0.3-1.1 keV,**** **
**1.1-2.8 keV**
**2.8-9.0 keV**

**Simulated 20 ks Con-X northern halo observation, 0.3-2.0 keV.**

**O VII and O VIII region.**
**Well resolved triplet,**
**high S/N in continuum.**

**With calorimeter ~2-eV resolution we can determine **
**T, n****e**** t, [Z/H], v****HOT**** accurately in many extended winds (not just M82).**

## Hot gas around normal disk galaxies

**Normal spiral galaxies**

**Example starburst**
**galaxy with superwind**

**Red: H-alpha (WIM),**** ****Green: R-band (starlight),**** ****Blue: Diffuse soft X-ray (3 million deg gas).**
**The region covered by each image is 20 x 20 kpc. Intensity scale in square-root. **

- NGC 891

- NGC 4013

- NGC 4217

- NGC 3628

- courtesy of D. Strickland (JHU)

## Interested in more Constellation-X Science?

## Available in PDF form at 

- Available in PDF form at
- constellation.gsfc.nasa.gov

## THANK YOU

- Please visit http://constellation.gsfc.nasa.gov
**Questions? Email me: annh@milkyway.gsfc.nasa.gov**

## Constellation-X Facility Science Team

**FST Steering Committee:** Harvey Tananbaum (SAO - Chair) Nicholas White (GSFC - Project  Scientist)  Ann Hornschemeier (GSFC -    Deputy Project   Scientist) Jay Bookbinder (SAO - Mission Scientist) Robert Petre (GSFC - Mission Scientist) Michael Garcia (SAO - SAO Science Lead) Steve Kahn (Stanford/SLAC - At-large)
**Instrument Product Team Leaders:**   HXT: Fiona Harrison (CalTech) Grating/CCD: Kathryn Flanagan (MIT) Calorimeter: Richard Kelley (GSFC) SXT: Rob Petre (GSFC)
**FST At-Large Members, Science**:  Scott Anderson (U. Washington)Keith Arnaud (U. of Maryland) Steven Allen (Stanford)  Jill Bechtold (U. of Arizona) Mitchell Begelman (U. of Colorado) Elliot Bloom (SLAC) Joel Bregman (U. of Michigan) Claude Canizares (MIT) Andy Fabian (Institute of Astronomy - UK) Gabriele Ghisellini (Osservatorio Astronomico di Brera-Italy) John Hughes (Rutgers U.) Duane Liedahl (Lawrence Livermore National Lab) Abraham Loeb (Harvard University)Frank Marshall (GSFC) Giorgio Matt (Universit‡ degli Studi Roma Tre-Italy) Bruce Margon (STScI) Richard Mushotzky (GSFC) Robert Rosner (U. Chicago) Chris Reynolds (U. of Maryland) Michael Shull (U. of Colorado)