Mass%20Estimate%20of%20Black%20Hole%20Candidates%20GRS%201758-258%20and%20GX339-4%20Based%20on%20a%20Transition%20Layer%20Model%20of%20the%20Accretion%20Disk%20and%20a%20Search%20for%20X-ray%20Jets%20in%20GRS%201758-258

1
Mass Estimate of Black Hole Candidates GRS
1758-258 and GX339-4 Based on a Transition Layer
Model of the Accretion Disk and a Search for
X-ray Jets in GRS 1758-258
Nathan D. Bezayiff, David M. Smith University of
California Santa Cruz
Santa Cruz Institute for Particle Physics Seminar
May 23, 2006
2
GX 339-4 and GRS 1758-258 areLow Mass X-Ray
Binary Systems

1. Companion Star is smaller than or equal to our
   sun.
2. Roche Lobe is the most common type of accretion.
3. If the point where the gravitational attraction
   between the two stars is equal (Inner Lagrange
   Point) occurs near the surface of the Companion
   Star, matter will be stripped from the Companion
   Star into an Accretion Disc that forms around the
   Compact Object.
4. Matter falling into the black hole converts about
   half its graviational binding energy to radiation
   via viscosity the other half will be released
   near the surface of the star.

3
Companion Star
Jets ?
Compact Object
?
Accretion Disc
Gravitational Attraction Between Both Stars
equal
From http//lheawww.gsfc.nasa.gov/still/research/
corr.html
4
Motivation For Development of the Transition
Layer Model to Determine the Mass of Black Holes

• 1. In a Low-Mass X-Ray Binary System, no
  knowledge of any of the parameters of the
  companion are required.
• 2. The parameters required to determine the
  mass of a black hole only depend on the Energy
  Spectrum Power Law Index and Power Density Quasi
  Periodic Oscillation Frequency.
• 3. GRS 1758-258, 1E 1740.7-2942, and GX 339-4
  are black holes where companion information does
  not exist. Hence their mass must be determined by
  another method.
• 4. May help to classify objects as neutron
  stars or black holes easier. If saturation of the
  Power-Law Indices is observed, the object is a
  black hole. If no saturation of the Power-Law
  Indices are observed, the object may be a neutron
  star.

5
Proportional Counter Array of Rossi X-Ray Timing
Explorer Provides Timing, Energy Spectra
Energy range 2 - 60 keV Energy resolution lt
18 at 6 keV Time resolution 1 microsec
Spatial resolution collimator with 1 degree
FWHM Detectors 5 proportional counters
Collecting area 6500 square cm Layers 1
Propane veto 3 Xenon, each split into two 1
Xenon veto layer
6
Obtaining the PLI and QPO from a given
observation for GRS 1758-258
First, Get the Power Law Index
?
Power Law Component
?
Interstellar Absorption
Residuals Normalized counts/sec/keV
Channel Energy (keV)
7
Obtain the Quasi Periodic Oscillation Frequency
in the Power Density Spectra
QPO
Power Density (Rms/Mean)2/Hz
Frequency (Hz)
8
(PLI) Power Law Index-Quasi Periodic Oscillation
(QPO) curve
Power Law Index
?
Harmonic Pair?
Quasi-Periodic Oscillation (QPO) freq (Hz)
9
TRANSITION LAYER MODEL (VERY BASIC)
1. The Optical Depth (t) is related to the
accretion rate (dM/dt)
2. The Power Law Index, G is related to the
Optical Depth,t.
3. The Power Law Index is related to dM/dt
4. The QPO frequency is related to the Transition
Layer Outer Radius
5. The Transition Layer is Related to dM/dt
6. Thus, sine both G and n are both related to
dM/dt, they are related to each other.
10
QuasiPeriodic Oscillation Correlations of two
black holes related by shift in QPO frequency,
n2(m1/m2) n1
Best Fit Mass GRS 1758-258 2.3 .00m
GRS 1915 105
GRS 1758-258
11

• The Fit is Poor and the Curve is the Wrong
• Shape

2. There are two more free parameters
we can adjust A, d. They are found from
the relation between t and the Reynolds
number g, tA gd.
3. We Can Allow A, d, and the mass to Vary
and fit them freely for the Black Hole as
done for GRS 1915105 (TF04)
12
1. If we assume GRS 1758-258 and GRS1915105
have the same tA gd (A1.0, d
1.25) then the best fit mass is
m2.3.0m 3. If t(g) is different for GRS
1758-258, our best fits have A1.0, d
is 0.95), and the best fit mass is m9.3.05-3.3m
13
A, d are clearly important in the shift between
QPO-PLI Correlations from one black hole to
another. A, d, and the mass are not orthogonal.
Below, curve families of A, m, d.
Mass varies
A varies
d varies
A, mass constant
Mass, d constant
A, d constant
14
Reduced chi square space for GX339-4 One of
A,m,d is held constant at best fit
parameters.
d,Constant, Mass-A varied
A constant, M- d varied
d
A
Mass (M )
Mass (M)
Mass constant, d-A varied
d
A
15
Transition Layer Model More Complicated for GX
339-4
Power Law Index
Quasi-Periodic Oscillation (QPO) freq (Hz)
16
GX 339-4 Blue Count Rate gt 500 cts/sec Red lt 500
Cts/secBlue 2002 Outburst, Red is 2004, 2003,
2005 Outburst
Power Law Index
Quasi-Periodic Oscillation (QPO) freq (Hz)
17
GX 339-4 Low, Best Fit ParametersA 0.75,
Mass2.68M, d1.6
2.05 0.0 M
Power Law Index
Quasi-Periodic Oscillation (QPO) freq (Hz)
18
GX 339-4 High, Best Fit ParametersA0.65,
Mass2.35 M, d2.35
2.66 0.04 0.05 M
Power Law Index
Quasi-Periodic Oscillation (QPO) freq (Hz)
19
CONCLUSIONS FOR TRANSITION LAYER
MODEL 1. Certain parameters need to be
better constrained in the TL model, i.e., A, d,
saturation 2. Wed like to do the analysis
considering the other harmonics as the
fundamental frequency. 3. GRS 1758-258 appears
to be the type of black hole that the transition
layer model may apply to. 4. The Transition
Layer Model predicts a possible neutron star mass
for GX 339-4. Better fits and saturation are
required to support this prediction.
20
Part II Search For X-Ray Jets in GRS 1758-258
21
Motivation For X-Ray Jet Search For GRS 1758-258

• 1. Persistent Radio Jets Have Been Seen in GRS
  1758-258.
• 2. A Persistent Extension Has Been Seen in
  Cygnus X-3.
• 3. Might GRS 1758-258 have X-ray jets too?

Extension
22
The Chandra HRC-I is excellent for Imaging X-Ray
Sources

• 1. 0.13 per pixel Resolution
• 2. Large uniform field of view (31 x 31 arc
  minutes)
• 3. Large uniform field of view (31 x 31 arc
  minutes)
• 4. High time resolution over the entire field of
  view (16 microseconds)
• 5. Low background (4 x 10-6 cts/s/arcsec)

Chandra Satellite
High Resolution Camera HRC-I
23
Raw Data From HRC-I
GRS 1758-258 Observation 2718
Each Pixel is 0.13
24
Fit Gaussians to Slices, Look For Unusual
Standard Deviations
Point Spread Function Sigma
Slice Angle (Degrees)
Heindl Astrophys J. 578,2 L125
25
Gaussian Fits of Slices Through Center Yield No
X-Ray Jets
1E 1740.7-2942 ?
GRS 1758-258 X
Cygnus X-3
AR Lacertae ?
26
Radio Jets Have Been Seen in GRS 1758-258.
Thus, We Looked For X-Ray Jets in Radio Centers
27
No Jets Found In Regions Corresponding To, or
Perpendicular To Radio Jets
South Lobe
North Lobe Signal/Noise 0.72
1.47 Ratio Counts/Area
1.07 1..34 of GRS 1758 7.66e-3 9. 6e-3
Core Brightness Needed for 3-Sigma
Detection Counts/Area 1.18 1..39
of GRS 1758 8.45e-3
9. 9e-3 Core Brightness
28
Finally, We Took Azimuthal Slices Around GRS
1758-258
18 arcsecs
29
We Found An Extension . . .
Signal/Noise Counts in
Counts/Area
12.2 arcsec2 region 136 Degrees
4.07 200 16.4 316 Degrees
2.90 177 14.5 Avg Background
---- 126 10.3
30
But It Is A Detector Artifact
Merged Data Roll Angle270
Merged Data Roll Angle90

• 1.The spacecraft orientation is 90 or 270
  degrees. If the extension was real, it should be
  present no matter how I orient the Satellite.
• 2. Upon rotating the satellite, the extension
  rotates also, so the extension must be part of
  the satellite.
• 3. From the Chandra Handbook, a ghost artifact,
  a secondary image, appears on one side of every
  source, due to the Saturation of the High Gain
  Amplifiers. The brightness of the ghost image is
  reported to be 0.1 of the source.
• 4. The fake jet is about 0.01 of the
  brightness of the center of the source.
• 5. Thus we conclude the extension is an artifact
  of the satellite.

31
Expected Signals if GRS 1758-258 Was Similar to
Other Black Holes

What Would The Size of the Jet Be?
What Would The Flux of the Jet Be?
BH Black Hole GRS is being compared to, PSPoint
Source or Central Compact Region, RRadius,
DDistance to compact object, Jsize of Jet in
Arcsecs, FFlux of Jet in ergs/sec/cm2
32
Black Holes Most Similar to GRS 1758-258
H1743-322
XTE J1550-564
M87
Cygnus X-3
33
GRS 1758-258
width X height
commentsH1743-322 1.88 X
1.88 ejected Cygnus X-3
5.88 X 2.35
persistent/ continuous XTE J1550-564
5.1 X 2.55
ejected M87 (with BH mass scaled)
1.48E-4 X 1.4E-5 persistent/
continuous M87 (without BH mass scake)
44,470 X 4,447 persistent/
continuous
Persistentappeared in all observations,
continuousconnected to central source,
ejectedseparated from central source

• GRS_jet_flux
  WebPimms cts/
  Could we
• X-Ray Jet Flux ergs/sec/cm2 cts/sec
  arcsec2 detect
  this?
• H1743-322 1.32e-14
  9.55e-5 1.55
  No
• Cygnus X-3 3.27e-12
  0.023 95.8
  Yes
• XTE J1550-564 5.21e-13
  3.76e-3 139.5
  Yes
• M87 6e-8
  452.7 1.6e16
  Yes
• Radio Jet Flux
• H1743-322 e-17
  7.23e-8 1.0e-3 No
• Cygnus X-3 2.46e-12
  0.018 75.18
  Yes
• XTE J1550-564 1.73e-13
  1.23e-3 45..92
  Yes
• M87 (no radio data)

34
Conclusions For X-Ray Jet Search of GRS 1758-258

• 1. No Jets Were Found With Chandra Observations.
• 2. If GRS 1758-258 Was Similar to Black Holes
  M87, Cygnus X-3, or XTE J1550-564, We Should
  Have Seen X-Ray Jets Based on Rough Estimates. If
  GRS 1758-258 is More Similar to H1743-322, We
  Would Not Have Seen X-Ray Jets.
• 3. The Extension We Found Was a Property of the
  Chandra HRC-I Detector.