The Next Nearest BH Open Univ Dec 2004

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M31 - The Nearest Extra-Galactic SMBH
Michael Garcia, Smithsonian Astrophysical
Observatory Lorant Sjouwerman, NRAO
Chandra HRC
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M31 - The Nearest X-Galactic SMBH
PLUS Frank Primini, SAO Ben Williams, Penn
State Albert Kong, MIT Manuel Torres, SAO Jose
Galache, SAO Ramesh Narayan, Harvard Fulvio
Melia, U of A Feng Yuan, Shanghi Steve Murray,
SAO Phil Kaaret, U of Iowa Pauline Barmby,
SAO Danny Steeghs, SAO
Chandra HRC
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Chandra Observations of M31 Goals

• Study Black Hole Nova. 80 Galactic SXTBH. Do
  ASM like Survey, Orbital Periods, Spectral
  changes, BH Spin w/ Con-X ala CXO
• M31 SMBH
• Population studies (HMXB, LMXB, SNR. helped by
  common D, low AV
• Surprises!
• Separate bulge sources, resolve SNR- RESOLUTION
  Helps!

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Punch LineM31 Compared to Other Nearby SMBH

• LARGEST Bondi Radius!
• Extreme Quiescence
• M31 near to SgrA, LRsecure and severe
  constraints non-radiative accretion.
• Well detected, variable X-ray and Radio source.

Severe constraints
Secure accretion rate
Secure accretion rate
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Our Campaign ACIS Followup of Transients

• Most transients in bulge, ACISHRC obs
  concentrated
• AO1,2,3,5,7 107 separate obs, S574ks!
  141/814ks!!
• Time 50/50 GO/GTO multi-year program not
  possible w/o GTO time!
• 7 year span yeilds numbers of SXT vs
  persistent, duty cycles.
• 574 ks sensitive measure of M31, LF, SNR, etc.

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PN/SNR XRB Associations

• Kong etal 2002 8 PNs w/ Lx1037 (!)
• Williams etal 2004
• Register with LGS to 0.25, OIII,SII, Ha.
• NOT matches! Near misses Prob 1
• X-ray spectra/timing XRBs
• What are they?
• Dont Know! optical spectra will help (no
  examples in MW - survey eased in M31)

OIII
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One New Example in MW!
Optical w/ contours
Radio

• Gallo, Fender etal 2005 Nature
• Cyg X-1 radio/optical bubble blown by jet
• Separation _at_M31 1 arcsec as seen in PN/SNR
  XRBs
• Optical spectra could tell!

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M31 SMBH
P1
P3 M31
P2
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Kong etal 2002 ACIS Mosaic Clear Diffuse
emission In central region
Kormendy and Bender 1999 Rare Double Nucleus,
torus 3 x 107 M SMBH _at_P2 peak 1.4 x 108 M _at_P3,
Bender etal 05
Bondi accretion rate? Bondi Radius? Accretion
(radiation) efficiency? jets? Position of Crane
1992 pt radio source? (within 0.5, accurate to
0.15)
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M31
Two HST/Chandra Matches of Globular Clusters
MIT213 Optically Bright inner 7 new,
Barmby, faint Registration to 0.1 (now
use LGS to lt0.1)
Optical Image
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M31 - HRC and ACS to 0.1Garcia etal 2005 ApJ
50ks HRC image M31 error circle 0.1
radius Dashed line resolved source, 13 counts,
2.5s Above N1SSSdiffuse 13 counts 1036
ergs/sec
ACS image, HRC contours Separate (resolved)
contour at M31 Radio pt source in white
predates Discovery of double nucleus! (so
allowed smaller optical/radio error)
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M31 - ACIS and WF/PC2 to 0.1
WF/PC2 image with ACIS contours Countours
extending In dirextion of M31 Flux consistent
with HRC
35ks merged ACIS image M31 position error w/
0.1 radius M31 not cleanly resolved, but
some Extension towards it. ACIS pix 0.5. HRC
pix 0.125
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M31 - A06 HRC/VLA Movie
50ks HRC image
4 x 50 ks HRC images, simultaneous VLA MUCH
variability in M31 and field! Radio/X-ray may
distinguish Jets/ADAF
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M31 Simultaneous Radio/X-ray

• Chandra/VLA
• 4 obs spaced 1m
• VLA/A CXO/HRC
• Prelim light curves stats can be better
• No evidence for lt1 day variations, lt30
• Factor 2 decrease in months
• Radio anti-correlated?
• Runs test lt 2s (please repeat!)

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M31 Radio Variability

• 2 hour averages
• Factor 2 in 4 hours
• 20 RSCH at c!
• TB 5x109 K
• Scintillation?
• Jet Variability?
• If intrinsic, radio is not emission from a RIAF
• Sgr A also shows hour (but typically longer)
  variations

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M31 Bulge Diffuse Emission
Li and Wang, U Mass Amherst, 2006
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Clear Structure

• Li Wang 06
• 200ks, ACIS
• 37 obs merged
• 0.5-1.0keV,
• 1.0-2.0keV,
• 2.0-4.0keV
• T0.1,0.3,0.6 keV (Takahashi 04, Dosaj 02)
• Structured, SNR shocks?
• Outflow?

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Softest, Central Diffuse

• 52ks ACIS-S only
• 4, lt2001 obs
• 0.2-0.5keV,
• 0.5-2.0keV,
• 2.0-7.5keV
• Structure NOT due to scattering from point
  sources
• 0.3keV dominates Emission Measure and density,.

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Diffuse at M31

• Bondi Radius 4
• No obvious signature of flow
• Bender etal 2005 P3 200 A0 stars, new SFR, 200
  Myears, 4000 Msun IMF 2e-5 Suns/year
• MBondi 1e-4 Suns/year
• 20 form stars?
• How does it cool?
• VERY high efficiency

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Radio/X-ray Diffuse Interactions
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X-ray Radio
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Radio/X-ray Diffuse Interactions?
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SummaryM31 Compared to Other Nearby SMBH

• Variable X-ray (months), Radio lt1day
  scintillation?
• Extreme Quiescence RIAF
• M31 near to SgrA, LRsecure and severe
  constraints LARGEST Bondi radius of any SMBH!!
• Speculation T0.3keV M31, 1.5keV SgrA -
  Selection effect? AV30, low T hidden?
• M31/SgrA Lx1000, Lr0.2 More chance to see
  ISCO 45ks in M31
• May be correlation between diffuse radio and soft
  X-ray emission shocks or bubbles?

Severe constraints
Secure accretion rate
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END extra slides
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Summary Chandra M31 Campaign, Some Surprises
and M31

• 7 Year Synoptic program Modest exposures, but
  sum 574ks, could obtain 1 Msec if continued
• Many Transients found 45 total, Williams 2005
• SXT Counterparts - 6 ORBITAL PERIODS, 5 more in
  AO7
• Surprises
• N(NS) N(BH) expect N(NS) gt N(BH)
• X-rays near PNebula/SNR? Ejected XRBs? Jets?
• Resolved SNR w/ embedded XRB
• M31 RBH resolved, Severe and Secure
  constraints
• M31 X-ray/Radio Variablity Jets or ADAF?

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Radio Holes In Diffuse X-ray?
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Duty Cycles (real measurments!)Williams etal
2005 ApJ

• 45 Transients
• First 2.8y ACISHRC XMM
• Light curves, HID, spectra, decay times
• High concentration in bulge
• Measurements, limits of duty cycles
• Lowest are 2 (vs 1 canoncial)

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Transients Williams etal 2003 (surprise 1)

• Nov 99 June 02, 2.5 years, HRC-I only -
  covering FULL disk
• 17 Transients in 17 Snapshots concentrated in
  bulge
• 1 new source per obs, 100 persistent (NS) in
  bulge
• Transients concentrate in Bulge region likely
  LM -gt BH XRN?
• SURPRISE IF Duty Cycle of BH 1 (MW) -gt similar
  BH and NS
• Evolutionary calcs often predict NSgtgtBH !
  (re-discovery of MW numbers)

Williams 2005 ApJ submitted, 45(!) transients,
ACIS, XMM, poster HERE
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Transient NSA Sources

• 3 of 45 fit NSA, rest fit DBB/PL
• IF NS in M31 Rgt105 km not in M31!
• If R10km, dlt100pc(!), Lx1030
• If WD, in MW Halo
• gt1 deg2
• Only repeated (107x !) survey to lt10-13
  erg/cm2/s (W.P.!)

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Softest, Central Diffuse

• 52ks ACIS-S only
• 4, lt2001 obs
• 0.2-0.5keV,
• 0.5-2.0keV,
• 2.0-7.5keV
• Structure NOT due to scattering
• T increases inwards?
• 0.3keV dominates Emission Measure and density,.

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Results 5 GHz VLA image

• Extended and resolved sources
• Point sources
• Variable, or steep-spectrum sources
• Polarized filaments?

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