# Presentation: 170604

## M31* - The Nearest Extra-Galactic SMBH

**M31* - The Nearest Extra-Galactic SMBH**

**Michael Garcia, Smithsonian Astrophysical Observatory**
**Lorant Sjouwerman, NRAO**

- Chandra HRC

- M. Garcia, OU, Dec 21 2004

## M31* - The Nearest X-Galactic SMBH

**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

- M. Garcia, OU, Dec 21 2004

## Chandra Observations of M31: Goals

- Study Black Hole Nova.  ~80% Galactic SXT=BH. 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!

- M. Garcia, OU, Dec 21 2004

## Punch Line:M31* Compared to Other Nearby SMBH

- “Extreme Quiescence”
- M31* near to SgrA*, LR=‘secure and severe’ constraints – non-radiative accretion.
- Well detected, variable X-ray and Radio source.

- Punch Line:M31* Compared to Other Nearby SMBH

- Secure accretion rate

- Severe constraints

- Secure accretion rate

- M. Garcia, OU, Dec 21 2004

## Our Campaign: ACIS Followup of Transients 

- Most transients in bulge, ACIS+HRC obs concentrated
- AO1,2,3,5,7... 107 separate obs, =574ks!  [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.

- M. Garcia, OU, Dec 21 2004

## PN/SNR +XRB Associations 

- Kong etal 2002 – 8 PNs w/ Lx~1037 (!)
- Williams etal 2004
- Register with LGS to 0.25’’, O[III],S[II], H
- NOT matches! Near misses – Prob 1%
- X-ray spectra/timing ~ XRBs
- What are they?
- Don’t Know! optical spectra will help (no examples in MW - survey eased in M31)

- O[III]

- M. Garcia, OU, Dec 21 2004

## One New Example in MW!  

- Optical w/ contours

- Radio

- Gallo, Fender etal 2005 Nature
- Cyg X-1 radio/optical ‘bubble’ blown by jet
- Separation @M31 = 1 arcsec... as seen in PN/SNR + XRBs
- Optical spectra could tell!

- M. Garcia, OU, Dec 21 2004

## M31* SMBH

- ~3’

- Kormendy and Bender 1999
- Rare Double Nucleus, ‘torus’
- 3 x 107 M SMBH @~P2 peak
- 1.4 x 108 M @P3, Bender etal 05

- Kong etal 2002
- ACIS Mosaic – Clear Diffuse emission
- In central region

- Bondi accretion rate?   Bondi Radius?   Accretion (radiation) efficiency?  jets?
- Position of Crane 1992 pt radio source? (within 0.5’’, accurate to 0.15’’...)

- P1

-  P3
- M31*

- P2

- M. Garcia, OU, Dec 21 2004

## M31*

- Optical Image

- Two HST/Chandra Matches of Globular Clusters
- 	   MIT213 = Optically Bright
- 	‘inner 7’ = new, Barmby, faint
- 	      Registration to ~0.1’’ (now use LGS to <0.1’’)

- M. Garcia, OU, Dec 21 2004

## M31* - HRC  and ACS  to 0.1’’Garcia etal 2005 ApJ

- M31* - HRC  and ACS  to 0.1’’Garcia etal 2005 ApJ

- 50ks HRC image
- M31* error circle = 0.1’’ radius
- Dashed line = resolved source, 13 counts, 2.5
- Above N1+SSS+diffuse
- 13 counts ~ 10^36 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)

- M. Garcia, OU, Dec 21 2004

## M31* - ACIS and WF/PC2 to 0.1’’

- 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’’

- WF/PC2 image with ACIS contours
- Countours extending
- In dirextion of M31*
- Flux consistent with HRC

- M. Garcia, OU, Dec 21 2004

## 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

- M. Garcia, OU, Dec 21 2004

## 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 <1 day  variations, <30%
- Factor 2 decrease in months
- Radio anti-correlated?
- Runs test < 2(please repeat!)

- M. Garcia, OU, Dec 21 2004

## 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

- M. Garcia, OU, Dec 21 2004

## M31 Bulge Diffuse Emission

- Li and Wang, U Mass Amherst, 2006

- M. Garcia, OU, Dec 21 2004

## Clear Structure

- Li & Wang 06
- ~200ks, ACIS
- 37 obs merged
- 0.5-1.0keV,
- 	1.0-2.0keV,
- 	2.0-4.0keV
- T=0.1,0.3,0.6 keV (Takahashi 04, Dosaj 02)
- Structured, SNR shocks?
- Outflow?

- M. Garcia, OU, Dec 21 2004

## Softest, Central Diffuse 

- 52ks ACIS-S only
- 4, <2001 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,.

- M. Garcia, OU, Dec 21 2004

## 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

- M. Garcia, OU, Dec 21 2004

## Radio/X-ray Diffuse Interactions

- M. Garcia, OU, Dec 21 2004

## X-ray                    Radio 

- M. Garcia, OU, Dec 21 2004

## Radio/X-ray Diffuse Interactions? 

- M. Garcia, OU, Dec 21 2004

## Summary:M31* Compared to Other Nearby SMBH

- “Extreme Quiescence” = RIAF
- M31* near to SgrA*, LR=‘secure and severe’ constraints LARGEST Bondi radius of any SMBH!!
- Speculation:  T~0.3keV M31*, ~1.5keV SgrA* - Selection effect? AV~30, low T hidden?
- M31*/SgrA*  Lx~1000, Lr~0.2: More chance to see ISCO = 45ks in M31*
- May be correlation between diffuse radio and soft X-ray emission – shocks or bubbles?

- Summary:M31* Compared to Other Nearby SMBH

- Secure accretion rate

- Severe constraints

- M. Garcia, OU, Dec 21 2004

## END – extra slides

- M. Garcia, OU, Dec 21 2004

## Summary: Chandra M31 Campaign, Some Surprises and M31*

- 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) > 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?

- M. Garcia, OU, Dec 21 2004

## Radio ‘Holes’ In Diffuse X-ray? 

- M. Garcia, OU, Dec 21 2004

## Duty Cycles (real measurments!)Williams etal 2005 ApJ  

- Duty Cycles (real measurments!)Williams etal 2005 ApJ

- 45 Transients
- First 2.8y ACIS+HRC +XMM
- Light curves, HID, spectra, decay times...
- High concentration in bulge
- Measurements, limits of duty cycles
- Lowest are 2% (vs 1% canoncial)

- M. Garcia, OU, Dec 21 2004

## Transients: Williams etal 2003 (surprise 1)

- 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 -> BH XRN?
- SURPRISE: IF Duty Cycle of BH ~1% (MW) -> similar # BH and NS
- Evolutionary calcs often predict #NS>>#BH ! (re-discovery of MW numbers)

**Williams 2005 ApJ submitted, 45(!) transients, ACIS, XMM, poster HERE**

- M. Garcia, OU, Dec 21 2004

## Transient NSA Sources

- 3 of 45 fit NSA, rest fit DBB/PL
- IF NS in M31 R>105 km – not in M31!
- If R=10km, d<100pc(!), Lx~1030
- If WD, in MW Halo
- >1 deg2
- Only repeated (107x !) survey to  <10-13 erg/cm2/s (W.P.!)

- M. Garcia, OU, Dec 21 2004

## Softest, Central Diffuse 

- 52ks ACIS-S only
- 4, <2001 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,.

- M. Garcia, OU, Dec 21 2004

## Results: 5 GHz VLA image

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

- 1’

- M. Garcia, OU, Dec 21 2004