ultraluminous x-ray sources with nustar & friends
TRANSCRIPT
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
M A T T E O B A C H E T T I W I T H D . B A R R E T, F. H A R R I S O N , J . M . M I L L E R , V. R A N A , D . W A LT O N , T H E N U S TA R U L X W G , A N D T H E N U S TA R T E A M D U B L I N , J U N E 1 9 T H, 2 0 1 4
U LT R A L U M I N O U S X - R AY S O U R C E S W I T H N U S TA R & F R I E N D S
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
W H Y “ U LT R A L U M I N O U S ” ?
LULX > 1039erg/s
Standard accretion limit on stellar-mass BHs
High BH mass?Super-Eddington accretion?
LEdd ⇡ 1.38 · 1038 M
M�erg/s
⇡ 1.38 · 1039 M
10M�erg/s
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
U L X S P E C T R A I N T H E X M M E R A
• Three main spectral shapes
• The same source can show one or more of these spectral states
• Broadened disk usually in low-luminosity sources
Sutton+13
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
• Three main spectral shapes
• The same source can show one or more of these spectral states
• Broadened disk usually in low-luminosity sources
Sutton+13
U L X S P E C T R A I N T H E X M M E R A
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
• Three main spectral shapes
• The same source can show one or more of these spectral states
• Broadened disk usually in low-luminosity sources
U L X S P E C T R A I N T H E X M M E R A
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
• Mostly Persistent!
• A soft excess(?)
• A hard turnover(?)
U L X S P E C T R A I N T H E X M M E R A
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
S P E C T R A L P R O P E R T I E S O F U L X S ( < 1 0 K E V )
• Mostly Persistent!
• A soft excess(?)
• A hard turnover(?)
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
S P E C T R A L P R O P E R T I E S O F U L X S ( < 1 0 K E V )
• Standard disk cut at the ISCO? (IMBH! e.g. Miller+04)
• Blurred emission lines? (e.g. Caballero-Garcia+10)
• A partially covered disk? (e.g. Gladstone+09)
• A soft deficit? (e.g. Gonçalves+06)• Mostly Persistent!
• A soft excess(?)
• A hard turnover(?)
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
S P E C T R A L P R O P E R T I E S O F U L X S ( < 1 0 K E V )
• Standard disk cut at the ISCO? (IMBH! e.g. Miller+04)
• Blurred emission lines? (e.g. Caballero-Garcia+10)
• A partially covered disk? (e.g. Gladstone+09)
• A soft deficit? (e.g. Gonçalves+06)
• A cutoff? (e.g. Stobbart+06)
• A turnover due to a broadened iron complex? (e.g. Caballero-Garcia+10)
• A second disk component? (e.g. Miller+13)
• A conspiracy? An illusion?
• Mostly Persistent!
• A soft excess(?)
• A hard turnover(?)
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
P O S S I B L E M O D E L S B E F O R E N U S TA R
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
P O S S I B L E M O D E L S B E F O R E N U S TA R
• Standard low/hard state: low T, powerlaw. Below Eddington (-> implies IMBH)
• Reflection-dominated (Caballero-García & Fabian ’10)
• “Ultraluminous state” (Gladstone et al. 09)? Large “cold” corona, disk hidden -> favors stellar mass
• slim, or p-free, disk (Ebisawa et al, Kawaguchi et al.): deviation from SS73’s temperature-radius relation. Super-Edd accretion possible.
• beaming and outflows: large apparent luminosity due to beaming.
• “Patchy disks”
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
P O S S I B L E M O D E L S B E F O R E N U S TA R
• Standard low/hard state: low T, powerlaw. Below Eddington (-> implies IMBH)
• Reflection-dominated (Caballero-García & Fabian ’10)
• “Ultraluminous state” (Gladstone et al. 09)? Large “cold” corona, disk hidden -> favors stellar mass
• slim, or p-free, disk (Ebisawa et al, Kawaguchi et al.): deviation from SS73’s temperature-radius relation. Super-Edd accretion possible.
• beaming and outflows: large apparent luminosity due to beaming.
• “Patchy disks”
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
T H E N U S TA R U L X P R O G R A M
• ~10 ULXs to study (6 this year)
• For 2012-2013, a Large Program XMM+NuSTAR (~400ks), + Suzaku, Chandra
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
T H E N U S TA R U L X P R O G R A M
• ~10 ULXs to study (6 this year)
• For 2012-2013, a Large Program XMM+NuSTAR (~400ks), + Suzaku, Chandra
Harrison et al. 2013
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
• Sources were selected for flux and hardness in the XMM band
• Most sources of the sample historically in the hard and soft ultraluminous states
T H E N U S TA R U L X P R O G R A M
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
• Sources were selected for flux and hardness in the XMM band
• Most sources of the sample historically in the hard and soft ultraluminous states
T H E N U S TA R U L X P R O G R A M
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
• Sources were selected for flux and hardness in the XMM band
• Most sources of the sample historically in the hard and soft ultraluminous states
T H E N U S TA R U L X P R O G R A M
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
N G C 1 3 1 3 X - 1
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
N G C 1 3 1 3 X - 1
Bachetti+13, ApJ
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
C U T O F F S , C U T O F F S E V E R Y W H E R E
ALL sources in our sample show a cutoff above 10 keV
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
C U T O F F S , C U T O F F S E V E R Y W H E R E
ALL sources in our sample show a cutoff above 10 keV
Ho IX X-1
N1313 X-1
Cir ULX5IC 342 X-1
IC 342 X-2
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Ho II X-1
Bachetti+13, Walton+13, Walton+14, Rana+14
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M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
E X C E S S E S , E X C E S S E S E V E R Y W H E R E ( ? )
Low energy: a disk-like component is detected in most sources below 1 keV.
High energy: In most cases the cutoff is not correctly described by single-kT Comptonization
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
E X C E S S E S , E X C E S S E S E V E R Y W H E R E ( ? )
Low energy: a disk-like component is detected in most sources below 1 keV.
High energy: In most cases the cutoff is not correctly described by single-kT Comptonization
IC 342 X-1
N1313 X-1
N1313 X-1
Bachetti+13, Rana+14
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
• Several sources showed a fast (~weeks) evolution of spectral shapes.
• Short-term variability appears mostly in the soft intermediate and broad disk states (as previously known).
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VA R I A B I L I T Y, VA R I A B I L I T Y E V E R Y W H E R E ( ~ )
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
• Several sources showed a fast (~weeks) evolution of spectral shapes.
• Short-term variability appears mostly in the soft intermediate and broad disk states (as previously known).
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Ho IX X-1
N1313 X-2
Cir ULX5
Ho IX X-1
Cir ULX5
N1313 X-2
VA R I A B I L I T Y, VA R I A B I L I T Y E V E R Y W H E R E ( ~ )
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
• Several sources showed a fast (~weeks) evolution of spectral shapes.
• Short-term variability appears mostly in the soft intermediate and broad disk states (as previously known).
VA R I A B I L I T Y, VA R I A B I L I T Y E V E R Y W H E R E ( ~ )
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
• Several sources showed a fast (~weeks) evolution of spectral shapes.
• Short-term variability appears mostly in the soft intermediate and broad disk states (as previously known).
VA R I A B I L I T Y, VA R I A B I L I T Y E V E R Y W H E R E ( ~ )
N5907 X-1
Walton+ in prep.
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
VA R I A B I L I T Y- W H AT W E H AV E L E A R N E D F R O M I T
• Temperature-luminosity relation deviates from SS disk in Cir ULX-5:
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• Spectral evolution highly non-standard
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M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
VA R I A B I L I T Y- W H AT W E H AV E L E A R N E D F R O M I T
• Temperature-luminosity relation deviates from SS disk in Cir ULX-5:
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• Spectral evolution highly non-standard
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Walton+13, Walton+14
Ho IX X-1
Cir ULX5
L / T↵,↵ ⇠ 1.7
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
S U M M A R Y O F T H E P R O G R A M
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
S U M M A R Y O F T H E P R O G R A M
• Sample of ULXs observed:
• NGC 1313 X-1, X-2 (XMM, NuSTAR, Chandra) -> Bachetti+13 ApJ, Miller+14 ApJL
• Cir ULX-5 (XMM, NuSTAR) -> serendipitous, Walton+13, ApJ
• IC 342 X-1, X-2 (XMM, NuSTAR) -> Rana+14, sub.
• Holmberg IX X-1 (or M81 X-9) (XMM, NuSTAR, Suzaku) -> Walton+14, acc.
• NGC 5204 X-1 (XMM, NuSTAR, Chandra) -> Mukherjee+ in prep.
• NGC 5907 X-1 (XMM, NuSTAR, Suzaku) -> Walton+ in prep.
• Holmberg II X-1
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
S U M M A R Y O F T H E P R O G R A M
• Sample of ULXs observed:
• NGC 1313 X-1, X-2 (XMM, NuSTAR, Chandra) -> Bachetti+13 ApJ, Miller+14 ApJL
• Cir ULX-5 (XMM, NuSTAR) -> serendipitous, Walton+13, ApJ
• IC 342 X-1, X-2 (XMM, NuSTAR) -> Rana+14, sub.
• Holmberg IX X-1 (or M81 X-9) (XMM, NuSTAR, Suzaku) -> Walton+14, acc.
• NGC 5204 X-1 (XMM, NuSTAR, Chandra) -> Mukherjee+ in prep.
• NGC 5907 X-1 (XMM, NuSTAR, Suzaku) -> Walton+ in prep.
• Holmberg II X-1
• (+ HLX-1, M82 X-1, M51, ...)
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
S U M M A R Y O F T H E P R O G R A M
• Sample of ULXs observed:
• NGC 1313 X-1, X-2 (XMM, NuSTAR, Chandra) -> Bachetti+13 ApJ, Miller+14 ApJL
• Cir ULX-5 (XMM, NuSTAR) -> serendipitous, Walton+13, ApJ
• IC 342 X-1, X-2 (XMM, NuSTAR) -> Rana+14, sub.
• Holmberg IX X-1 (or M81 X-9) (XMM, NuSTAR, Suzaku) -> Walton+14, acc.
• NGC 5204 X-1 (XMM, NuSTAR, Chandra) -> Mukherjee+ in prep.
• NGC 5907 X-1 (XMM, NuSTAR, Suzaku) -> Walton+ in prep.
• Holmberg II X-1
• (+ HLX-1, M82 X-1, M51, ...)
• Data analysis ongoing
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
C O N C L U S I O N S
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
C O N C L U S I O N S
• Thanks to NuSTAR, degeneracy of spectral models reduced drastically.
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
C O N C L U S I O N S
• Thanks to NuSTAR, degeneracy of spectral models reduced drastically.
• Observed ULXs show common features (low-T cutoff, low-T disk or p disk-like spectra)
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
C O N C L U S I O N S
• Thanks to NuSTAR, degeneracy of spectral models reduced drastically.
• Observed ULXs show common features (low-T cutoff, low-T disk or p disk-like spectra)
• No clear emission lines
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
C O N C L U S I O N S
• Thanks to NuSTAR, degeneracy of spectral models reduced drastically.
• Observed ULXs show common features (low-T cutoff, low-T disk or p disk-like spectra)
• No clear emission lines
• The hard state-like model is ruled out in all of them, as is the reflection-dominated regime in its simplest form. Spectrum more similar to “non-standard” very luminous BHs.
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
C O N C L U S I O N S
• Thanks to NuSTAR, degeneracy of spectral models reduced drastically.
• Observed ULXs show common features (low-T cutoff, low-T disk or p disk-like spectra)
• No clear emission lines
• The hard state-like model is ruled out in all of them, as is the reflection-dominated regime in its simplest form. Spectrum more similar to “non-standard” very luminous BHs.
• An excess from single-component Comptonization?
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
C O N C L U S I O N S
• Thanks to NuSTAR, degeneracy of spectral models reduced drastically.
• Observed ULXs show common features (low-T cutoff, low-T disk or p disk-like spectra)
• No clear emission lines
• The hard state-like model is ruled out in all of them, as is the reflection-dominated regime in its simplest form. Spectrum more similar to “non-standard” very luminous BHs.
• An excess from single-component Comptonization?
• -> No standard BH state. Favored interpretation quasi- or super-Eddington accretion in massive StMBHs
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
F U T U R E P L A N S
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
F U T U R E P L A N S
• Accepted (Swift+)XMM+NuSTAR program to sample more spectral states in NGC 1313 X-[12]
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
F U T U R E P L A N S
• Accepted (Swift+)XMM+NuSTAR program to sample more spectral states in NGC 1313 X-[12]
• New observations of NGC 5907 X-1 and other sources already planned
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M
M A T T E O B A C H E T T I T H E N U S TA R U L X P R O G R A M