A short review of the talks and posters presented

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A (short) review of the talks and posters
presented

• Randall Smith
• JHU NASA/GSFC

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Spectroscopy puts most of the physicsinto
X-ray astrophysics

• Claude Canizares

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1895 ApJ, 1, 1

• A. A. Michelson on how to measure spectral lines
  emitted in solar prominences

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Synthesize, dont Summarize

• Methods Models
• Accretion (WA, Fe K)
• Stars flares FIPs, O (-type) my!
• Expect the Unexpected
• Future of X-ray Spectroscopy

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What didnt we talk about? (much)

• SNRs (except Dewey) and we clearly need to
  re-observe Cas A in 6-7 years
• Clusters (except Peterson, Behar) although
  absence of cooling flows a blockbuster also
  found vturblt30 km/s with a 300 km/s spectrometer!

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What didnt we talk about? (much)

• SNRs (except Dewey) and we clearly need to
  re-observe Cas A in 6-7 years
• Clusters (except Peterson, Behar) although
  absence of cooling flows a blockbuster also
  found vturblt30 km/s with a 300 km/s spectrometer!
• We need non-dispersive X-ray spectra!

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Methods Models

• Some things are easy. Thank goodness!
• Identifying ion parent of (most) lines
• Fe L shell lines easy to id strengths harder
• RRC features mostly easy to id as well.
• Doppler shifts (if ? known well need lab data!)
• But getting ?v to 3.7 km/s in EX Hya impressive
• Diagnostic line ratios of (strong) lines
• But watch out for LOS differences in models!

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Methods Models

• Others are hard
• Fitting high-resolution broad band spectra
• Measuring a faint continuum
• Determining an Emission or Absorption Measure
  Distribution (EMD, AMD)
• Creating a model simple enough to calculate but
  powerful enough to encapsulate data

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Methods Models

• Are we ready for a satellite which produces
  nothing but high-resolution X-ray spectra?

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Methods Models Analyzing high-resolution
spectra

• RGS, HETG, and LETG spectra all have more
  resolution elements than this projector!
• Methods Which converge? to the right value?
• Photon Clean, including bootstrap
• Line-Based Analysis
• absline
• Gaussian fits after continuum determination
• Adding components until ?2 stops dropping
• Continuum finding find line-free regions,
  assumed power-law, spline fit, other method?
• What constitutes a good fit?

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Methods Models Analyzing high-resolution
spectra

• RGS, HETG, and LETG spectra all have more
  resolution elements than this projector!
• Methods Which converge? to the right value?
• Photon Clean, including bootstrap
• Line-Based Analysis
• absline
• Gaussian fits after continuum determination
• Adding components until ?2 stops dropping
• Continuum finding find line-free regions,
  assumed power-law, spline fit, other method?

What is a good fit?
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Methods Models Analyzing high-resolution
spectra

• Is the biggest problem
• atomic data? (20-30 correlated errors)
• calibration? (3-15 correlated errors)
• insufficient counts (what metric?)
• methodology? (unknown...)

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Methods Models

• Accessing data getting easier
• BiRD for XMM RGS data
• http//xmm.esac.esa.int/BiRD/
• XATLAS for HETG stellar data
• http//cxc.harvard.edu/XATLAS
• Profit for GUI spectral viewing
• with ATOMDB or XSTAR line ids!
• http//heasarc.gsfc.nasa.gov/software/profit
• ( CIELO for RGS/Sy1.5, HotGAS for HETGS)

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Accretion Introduction

• Ubiquitous process
• SMBH
• Galactic BH
• X-ray (NS) binaries
• WD (CVs baby Seyferts that become SSS when the
  corona collapses...)
• Dynamic! (Winds, WA, etc)
• M, Macc, Mwind, Router, Rinner, Spin
• Inclination, Magnetic geometry

.
.
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Accretion Questions, Asked or Answered

• RRCs prove photoionization is the dominant
  process in some parts of accretion flows.
• Broad Fe K? lines in some AGN are real
• But can we really measure the BH spin?
• Soft X-ray excess coincides with optical NLR
• WA Clumpy or a continuous distribution?
• Can we tell? Are models holding us back, or
  calibration, or the data?
• Some X-ray components match UV ones (e.g NGC
  7469), and they respond to changes in the source
  flux.

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Accretion Questions, Asked or Answered

• Hot Absorbers at High Velocities
• Do they exist? Are we missing a giant component
  of mass outflow?
• Regardless, X-ray observations show this
  component dominates UV flows ( gt 90) for nearby
  AGN.
• NELG spectra not so flat (?? 1.7-1.8, not 1.4),
  no disk reflection seen (NGC 2110, 3C445)

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Stars Flares FIPs O (-type) My!

• Static loop models have DEM ? T1.0-1.5
• Observations show DEM ? T4.0
• Which agrees with dynamic loop models
• Flares in X-ray may be in optical or not
• Abundances can change during flare.
• CTTS seem to show accretion as well
• Weak Fe K? seen in HR 9024 flare reflection
  model agrees with loop geometry.

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Stars Flares FIPs

• (I)FIP is
• Solved
• Mysterious
• Unexplained

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Stars Flares FIPs

• (I)FIP is
• Solved
• Mysterious
• Unexplained
• Confusing all those not working in stars...

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Hot Stars Controversy in the offing?

• O star lines are broad symmetric(ish)
• Resonant scattering?
• Opacity?
• Or from shocked protons CX, while the electrons
  remain cold

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Expect the Unexpected

• Measuring dust or molecular composition
• Ferrous vs ferric iron? With X-rays from the Crab
  nebula? Yes!
• Main limitation in seeing XAFS is data, both
  observational experimental.
• Did Alpha Cen A disappear? Nope, just got
  coolerside benefit of the LETGS
• X-rays can catch SS433s jet hitting a bump
• The hot gas seen at z0 is really in the Galactic
  halo.

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Future of X-ray Spectroscopy

• Velocity broadened lines detected with suggestion
  of both cold and collisional plasmas in the LLAGN
  M81 need resolution, EA!
• Detect redshifted iron lines from surface of NS,
  determine EOS need ...
• Track material falling into AGN via Fe K need...

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Future of X-ray Spectroscopy

• Velocity broadened lines detected with suggestion
  of both cold and collisional plasmas in the LLAGN
  M81 need resolution, EA!
• Detect redshifted iron lines from surface of NS,
  determine EOS need ...
• Track material falling into AGN via Fe K need...
• Con-X (and CAT) can give resolution, EA

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The Unified AGN Spectrum

• NGC 3783!