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The Search for Tidal Disruption Flares with with GALEX. Suvi Gezari California Institute of Technology & The GALEX Team California Institute of Technology, Laboratoire Astrophysique de Marseille Xi’an AGN 2006 -- October 21, 2006. Outline Capability of GALEX to Study Variability - PowerPoint PPT Presentation
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Suvi Gezari
California Institute of Technology
& The GALEX Team
California Institute of Technology,
Laboratoire Astrophysique de Marseille
Xi’an AGN 2006 -- October 21, 2006
The Search for Tidal Disruption Flares withThe Search for Tidal Disruption Flares with with GALEXwith GALEX
OutlineOutline
i. Capability of GALEX to Study Variability
ii. Tidal Disruption Flares: Theory and Observations
iii. Searching for Flares with GALEX
iv. Tidal Disruption Flare Discovered
v. Future Dedicated Time Domain Survey
Capabilities of GALEXCapabilities of GALEX
• Deep Imaging Survey, 80 deg2, >30 ksec (mlim ~ 25)• Observations obtained in 1.5 ksec eclipses• Time-tagged photon data (time resolution of 5 msec)• Large field of view (1.2 sq. deg.) and a large survey volume• Low sky background (source detection with 10 photons)• Simultaneous NUV (1750 - 2750 Å) and FUV (1350 - 1750 Å) imaging• Simultaneous R=100/200 NUV/FUV spectroscopic grism data
SDSSGALEX
A star will be disrupted when:Rp < RT ≈ R(MBH/M)1/3
Evans & Kochanek (1989)
Tidal Disruption EventsTidal Disruption Events
The bound fraction (< 0.5) of the stellar debris falls back onto the black hole, resulting in a luminous accretion flare.
Evans & Kochanek (1989)
t-5/3
Properties of a Tidal Disruption FlareProperties of a Tidal Disruption Flare
• For 106 - 108 M black holes, the stellar debris accretes in a thick disk (Ulmer 1999)
• Lflare≈LEdd=1.31045 M7 erg s-1
• Teff≈(LEdd/4RT2)1/4=3105 M7
1/12 K
• L(t)=(dM/dt)c2t-5/3
• dN/dt7/2MBH-1MBH
-1/4≈10-4 yr-1
(Wang & Merritt 2004)
Tidal disruption theory predicts rare but luminous flares that peak in the UV/X-ray domain, with decay timescales ~ months.
Why Search For Tidal Disruption Events?Why Search For Tidal Disruption Events?
• They are an unambiguous probe for supermassive black holes lurking in the nuclei of normal galaxies.
• The luminosity, temperature, and decay of the flare is dependent on the mass and spin of the black hole.
• They may contribute to black hole growth over cosmic times, and the faint end of the AGN luminosity function.
• Tidal disruption rates are sensitive to the structure and dynamics of the stellar galaxy nucleus.
Flares Detected by ROSATFlares Detected by ROSAT
The ROSAT All-Sky Survey (RASS) conducted in 1990-1991 was an excellent experiment to detect TDEs since it sampled 3x105
galaxies in the soft X-ray band (0.1 - 2.4 keV).
• Tbb = 6 - 12 x 105 K• Lx = 1042 - 1044 ergs s-1
• tflare ~ months• Event rate ≈ 1 x 10-5 yr-1 (Donley et al. 2002)
Properties of a tidal disruption event!
NLSy1
Sy1.9
non-active
Halpern, Gezari, & Komossa (2004)
Follow-up narrow-slit HST/STIS spectra confirmed the galaxies as non-active (Gezari et al. 2003).
Lflare/L10yr = 240
Lflare/L10yr = 6000
Lflare/L10yr = 1000
HST Chandra
STIS
STIS
• Narrow-line emission requires excitation by a persistent Seyfert nucleus.
• Seyfert nucleus in it inner 0.”1 was previously masked by H II regions in ground-based spectra
• The Chandra upper-limit on the nuclear X-ray luminosity is consistent with the predicted Lx from L(H) for LLAGNs, of ~ 9 x 1038 ergs s-1.
Li et al. (2002) modeled the event as the partial stripping of a low-mass star, or the disruption of a brown dwarf or giant planet.
Halpern, Gezari, & Komossa (2004)
NGC 5905
Gezari et al. (2003)
Search for Flares in the Deep Imaging SurveySearch for Flares in the Deep Imaging Survey
TOO observations with Chandra and Keck will probe the early-phase of decay of TDEs for the first time!
We take advantage of the UV sensitivity, temporal sampling, and large survey volume of GALEX.
Selection of Variable SourcesSelection of Variable Sources
is a measure of the dispersion in mag due to photometric errors
Identify the Host of the FlareIdentify the Host of the Flare
StarsQuasarsGalaxies
CFHTLS Colors & Morphology
Followed-up with TOO optical
spectroscopy
The most convincing candidates have inactive galaxy hosts!
Optically unresolvedo Optically resolvedx Xray detection Optically variable
Spectroscopic AGN
Archival Chandra ACIS detection in April 2002 with Lx ≈ 9.3x1042 ergs s-1
Presence of persistent Seyfert activity makes the tidal disruption scenario difficult to prove.
Jan 2006 MDM 2.4m spectrumL([O III]) = 9.4x1040 ergs s-1
Seyfert at z = 0.355!Some hosts show AGN activitySome hosts show AGN activity
AEGIS DEEP2 Keck Spectrum
Early-type galaxy with no evidence of Seyfert activity!
Confirmed Inactive Galaxy HostConfirmed Inactive Galaxy Host
Gezari et al. 2006, in press
UV Flare with tUV Flare with t-5/3-5/3 Decay Decay
t-5/3 The delay between tD and the peak of the flare implies MBH > 108 M.
tD
Gezari et al. 2006, in press
Properties of the Flare:T = 1 to 5 x 105 KL = 1044 to 1046 erg s-1
Macc > 0.3 Msun
In excellent agreement with theoretical predictions for a stellar disruption flare.
Simultaneous SED of the FlareSimultaneous SED of the Flare
CFHT SNLS
GALEX
Chandra(AEGIS)
Strongest empirical evidence for a stellar disruption event to date!
Gezari et al. 2006, in press
Constraints on MBH:MBH(t0-tD) > 1 x 108 Msun
MBH() ~ 1+1-.5 x 109 Msun
Critical upper limit on MBH for RT > Rs:Mcrit = 1 x 108 Msun (no spin)Mcrit = 8 x 108 Msun (O5 star)Mcrit = 8 x 108 Msun (with spin)
Upper limit on MBH for RBB > Rms:RBB < 4 x 1013 cmRms = 6Rg (no spin)Rms Rg (with spin)
If MBH > 108 Msun then RBB < 6Rg, and the black hole must have spin!
Disruption of a Star by a Disruption of a Star by a SpinningSpinning Black Hole Black Hole
2004.6 2004.9
NewNew Confirmed Flare from Inactive Galaxy Confirmed Flare from Inactive Galaxy
TOO VLT Spectrumcourtesy of Stephane Basa
Awaiting results from Chandra TOO!
z = 0.32
No Seyfert emission lines!
Dedicated Time Domain SurveyDedicated Time Domain Survey
• First time domain survey in UV• Designed to complement future ground-based TDS (PanStarrs, LSST)• All time-domain products, notably variable object alerts, will be immediately made public for community follow-up• Produce automated pipeline triggers to generate IAU and/or GCN circulars• Prevalence of UV-bright early evolution of flaring objects• The TDS may detect: supernovae, gamma-ray faint bursts, novae, macronovae, magnetic degenerate binaries, low mass x-ray binaries, chromospherically active stars, QSOs and AGNs, pulsating degenerates, luminous blue variables
Stay Tuned….Stay Tuned….
Candidate in D4Candidate in D42003 2005
2004.4 2006.0
Le Phare photo-z fits an elliptical galaxy at z=0.56
FUVflare=22.9
CFHT SNLScourtesy of Stephane Basa
Flare SED
Galaxy Host
• Chandra TOO X-ray observation in May 8, 2006 does not have a soft blackbody temperature.
• Follow-up spectrum of a ROSAT candidate also showed hard X-ray spectrum.
• Awaiting results from VLT optical spectrum.
T = 5 x 105 K
Image SubtractionImage Subtraction
Transient sources!
Method:1) Register images using a list of point source positions in both images.2) Subtract second image from reference image after polynomial spatial warping.3) Search difference image for sources above a threshold value with a correlation with the PSF of > 0.5.
Transient SourceTransient Source
Optically unresolved quasar!
CFHT SNLScourtesy of Stephane Basa
2005.0 2005.6
GALEX FUV band is sensitive to Rayleigh Jean’s tail of the soft X-ray blackbody emission.
A large K correction makes unextincted flare flux detectable by DIS out to high z.
6.5x10-4 yr-1 (MBH/106 M)-.25
(WM 2004)
E+S0 luminosity functionMBH = 8.1x10-5 (Lbulge/ L )0.18
(FS 1991, MT 1991, MF 2001)
Volume to which flares can be detected in a 10 ks DIS exposure
Yields 5 events yr-1 sq.deg-1(z ≤ 1)
Detection Rate with GALEXDetection Rate with GALEX
Transient SourceTransient Source
Optically resolved galaxy!
tmax≈2005.12
CFHT SNLScourtesy of Stephane Basa
2005.0 2005.6
SummarySummary
• Rich data set in spectral and temporal coverage when you combine GALEX + CFHT SNLS.
• Optical spectroscopy is necessary to confirm that flaring galaxies do not have an AGN, and we follow up our best candidates with Chandra TOO imaging.
• Legacy fields with multiwavelength coverage seem to be the most promising for identifying interesting variable sources.
• Can measure the distribution of masses and spins of dormant black holes.
• We have a new candidate with an inactive galaxy host confirmed by VLT TOO optical spectroscopy. We are awaiting the Chandra TOO observation results.
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