dynamical constraints on the mass of the black hole in a ulx
DESCRIPTION
No. Dynamical constraints on the mass of the black hole in a ULX. ^. Tim Roberts Jeanette Gladstone (Alberta) Andy Goulding , Mark Swinbank , Martin Ward (Durham) Mike Goad ( Leicester) Andrew Levan (Warwick ). ULX mass estimates. - PowerPoint PPT PresentationTRANSCRIPT
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Dynamical constraints on the mass of the black hole in a ULX^
No
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ULX mass estimates
Wide variety of methods used to make indirect measurements of BH mass (e.g. Zampieri & Roberts 2009)
X-ray luminosity & spectra Cool discs as IMBHs (e.g. Miller et al. 2003) Disc-dominated spectral models giving MBH ~
10 – 80 M (e.g. Vierdayanti et al. 2006)
Super-Eddington accretion models implying MBH < 100 M (e.g. Gladstone et al. 2009)
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ULX mass estimates (2)
X-ray timing measurements Scaling QPO, break frequencies gives IMBHs
(e.g. Strohmayer & Mushotzky 2009) But lack of variability in some ULXs argues for
small BHs (e.g Heil et al. 2009)
Optical constraints Counterpart magnitudes & colours (e.g.
Patruno & Zampieri 2010)
All degenerate, reliant on assumptions
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Dynamical masses: a heritage
To ‘weigh’ a BH – measure binary period and radial velocity shifts
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Early Cyg X-1 data (Bolton 1975) from stellar absorption lines
€
f (M) =MX
3 sin3 i
M* + MX( )2 =
PK*3
2πG
K*
P
€
f (M) =M*
3 sin3 i
M* +MX( )2 =
PKX3
2πG
From companion star:
From compact object:
Radial velocity curve of GRO J1655 from He II line (Soria et al. 1998)
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Extragalactic dynamical masses
Recently: two X-ray binaries outside our Galaxy with BH dynamical masses M33 X-7 (Orosz et al.
2007) – eclipsing system IC 10 X-1 (Prestwich et
al. 2007) – WR-BH binary with MBH ~ 24 – 33 M
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IC 10 X-1 radial velocity curve (Silverman & Filippenko 2009)
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Problems with doing this for ULXs…
Going from ~1 Mpc to several Mpc… Faint counterparts
(mv ~ 20.5 at best; typically > 24, Roberts et al. 2008)
Confused fields (stars & nebulae)
Observational challenge!
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HST data for Ho II X-1 (Kaaret et al. 2004)
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Previous attempts
Kaaret & Corbel (2009) – NGC 5408 X-1 6 VLT/FORS observations in 3 days No absorption lines from stellar companion;
broad He II (face-on system?)
Pakull, Grise et al. – NGC 1313 X-2 Early observations show Δv ~ 380 km s-1 in He
II line between epochs (Pakull et al. 2006) Follow-up in 2008/9 – no radial velocity
variations(?)
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Towards a ULX dynamical mass
We have been developing a programme to attempt to obtain ULX dynamical masses
3-step process:I. Identify counterparts from Chandra astrometry
and HST imaging (Jeanette Gladstone thesis; Gladstone et al. in prep.)
II. Obtain pilot optical spectroscopy observations to identify useful spectral features
III. Undertake the RV measurements campaign
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Best targets
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NGC 1313 X-2m555 = 23.3
NGC 5204 X-1m606 = 22.3
Ho IX X-1m555 = 22.5
Luminous ULXs (> 5 ×1039 erg s-1)
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Pilot spectroscopy results
Gemini G-MOS spectra obtained B600 grating
Gemini-S NGC 1313 X-2, 3 hr
Gemini-N NGC 5204 X-1, 0.8 hr Ho IX X-1, 1.5 hr
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New programme on Gemini
GN-2009B-Q-21: Ho IX X-1 (18.6 hours) 1.5 hours per observation
GS-2009B-Q-20: NGC 1313 X-2 (29.2 hours) 2.5 hours per observation
Strategy: request 10 observations performed on nightly intervals (when possible) Liu et al. (2009): ~ 6 day period in NGC 1313 X-2 Madhusudhan et al. (2008): 1 – 10 day periods
expected for small BHs in ULXsWeds 26th May 2010 Tim Roberts - ULX dynamical masses 11
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Data obtained
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NGC 1313 X-2: 1 obs. Oct, 9 in 13 nights Dec 2009
Ho IX X-1: 5 obs. late Dec 2009, 5 obs. Feb 2010.
Portion of 2-D spectrum from 26th Dec 2009 observation of Ho IX X-1
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He II 4686Å shifts relative to nebula
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Data from Ho IX X-1
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Periodicity?
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Best fit: P = 1.73 days, K = 77 km s-1
Reduced χ2 ~ 5
NOT PERIODIC
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Any better luck with NGC 1313 X-2?
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No.
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Best fit P = 3.01 days, K = 61 km s-1
Reduced χ2 ~ 4
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Is all lost?
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No – He II line profile is broad and variable on
timescales of days
Ho IX X-1 data
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Similarly for NGC 1313 X-2
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He II line profile broad and highly variable on timescales of days!
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Implications
He II emission from very close to ULX Solution: accretion disc reprocessing?
Broadening implies not completely face-on Line widths consistent with location very far out
in disc… …or a small velocity component in line-of-sight If this is from disc, can use limit from scatter in
velocity shift to put lower limit on BH mass
But other possibility: emission in wind?Weds 26th May 2010 Tim Roberts - ULX dynamical masses 19
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Mass limits
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NG
C 1
313
X-2
Ho
IX X
-12σ upper limits: K < 97 km s-1 (Ho IX X-1);
K < 182 km s-1 (NGC 1313 X-2)
6-day photometric
period
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One more thing…
Stack all 15 hrs observations to get high quality optical spectrum
Ho IX X-1 looks featureless, very blue - dominated by accretion disc light?
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NGC 1313 X-2: more interesting
Continuum less strong in 25 hrs on NGC 1313 X-2
Possible stellar features appearing at short wavelengths?
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Conclusions
Ambitious programme to constrain the dynamical mass of two ULXs attempted
He II line centroid varies; but not periodically Places no strong limit on BH mass
He II line is however broad and highly variable on timescales of days Could be from the accretion disc: implying source
close to face-on? Or from a wind?
Stacked spectra: very different counterpartsWeds 26th May 2010 Tim Roberts - ULX dynamical masses 23