GW Notes

April to August 2010

Notes & News for GW science Editors: P. Amaro-Seoane and B. F. Schutz

ISSN: 1868-1921

GW Notes was born from the need for a journal where the distinct communities in- volved in gravitational wave research might gather. While these three communities - Astrophysics, General Relativity and Data Analysis - have made significant collabora- tive progress over recent years, we believe that it is indispensable to future advance- ment that they draw closer, and that they speak a common idiom. Notes & News for GW science 4Spebr7 2010 7, September #4 URL: 1868-1921 ISSN: Schutz B.F. and Seoane Amaro P. Editors: (Albert-Einstein-Institut) Germany Potsdam Gravitationsphysik 14476 1 Mühlenberg für Am Max-Planck-Institut Publisher: http://brownbag.lisascience.org/lisa-gw-notes/ WNotes GW 1

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rmr ylsof cycles more or oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 -al [email protected] e-mail: Spain Barcelona, parells 08193 C5 Bellaterra, Torre UAB, Campus Ciències, de Facultat (CSIC-IEEC) l’Espai de Ciències de Institut Sopuerta F. Carlos OBSERVATIONS EMRI LISA FROM PHYSICS FUNDAMENTAL TO ROADMAP A olwdt aepors ntena future. be near can the that in avenues progress some make and to outcome develop followed scientific to the order maximize in to face tools information we necessary the this that all challenges from theoretical answer main observa- to the try EMRI discuss can we LISA finally, we future and, questions the scientific exploit what to the discuss tools we of of tions, some of development account the an in give made we progress Here, yet not experiments/observatories. regimes in other interaction by gravitational the proven and of nature details the the and like holes questions black physics things, of structure fundamental other of among understanding used, our be in can high advance that a to astronomy inspirals, extreme-mass-ratio wave so-called gravitational the for article source, tool this of precision In type third understood. the fully on yet focus not we processes physics and physical physics universe high-energy early to massive from a connected signatures into gravitational-wave object compact and stellar hole; a black of compact inspiral galactic subsequent many and collisions; capture galaxy the of binaries; outcome the find: as we mergers where potential, hole science black of massive terms in spectrum gravitational-wave rich- the the of probably part band, est gravitational-wave low-frequency next the National the in during operate US launched will the It be to decade. and expected Agency is that Space Administration) European Space and the Aeronautics between mission ob- joint gravitational-wave (a space-based future servatory a is Antenna Space Interferometer Laser The udmna hsc n EMRIs and physics Fundamental udmna hsc ihLISA with physics Fundamental WNtshglgtarticle highlight Notes GW Abstract WNotes GW

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11 oe esfrG science GW for News & Notes Notes & News for GW science 12 WNotes GW r ree oe n aesgicnl ihSga-oNieRto SR)(SNR (SNRs) Ratios Signal-to-Noise high significantly have & and more) even or yrs to nprln noaMHwt mass with MBH a into inspiraling where ( long quite that are fact LISA, the by on detectable based principle in is and EMRIs EMRIs, of by potential emitted the GWs the Physics, Fundamental of case the In sion. sim- a to using that idea estimated this been Applying has events it observations). model, EMRI GW cosmological the plified the from of inferred information be redshift cannot statistical (which provide to would up which distance surveys, luminosity the of measurements precise considered be can para- standard (which pro- Hubble observations been as EMRI the LISA has of correlating measurements it by direct possible Cosmology, precise are give that Regarding meter 2008) will Hogan, etc. which and IMBHs; MBH, (MacLeod of posed a existence solar into the million (IMBH) the for few BH detect evidence a to Intermediate-Mass to perhaps an up models; of formation masses galaxy inspiral for infor- for spins obtain implications MBH to has the progenitors; which their masses, of to distribution relation the their understand on to and mation order BHs in stellar nuclei galactic of in formation BHs the stellar informa- of spectrum obtain mass to the etc); about tion perturbers, massive relaxation, resonant segregation, (mass hssne ti xetd(e Ra,19b 97 n aakadCte,20) that 2007)) Cutler, measure and to Barack able and 1997a be 1995b, will (Ryan, LISA (see expected GWs is the it Then, sense, MBH. this the of region detailed field a gravitational carry strong the combed fully gets parameters: EMRI the of estimation (using section the estimated in in have appendix 2004) see Cutler, theory; and estimation (Barack parameter GW Cutler and Barack inspiral, of year orei h k sldage,and angle), (solid sky the in source where h rvttoa rhrznrdu fteMH o pnigBs ti ie by given is it BHs, spinning For region MBH. the the of mo- in radius r orbital horizon, from horizon comes or MBH emission gravitational the GW the EMRI to the close of tion most that account into Taking direction. spin MBH Horizon 30 z ∼ .UigatpclER ytmcnitn fa C ihmass with SCO an of consisting system EMRI typical a Using ). 0 S e . = o • 5 n ol esr h ubecntn obte hnoepretpreci- percent one than better to constant Hubble the measure could one , steiiileccentricity, initial the is eoe h B pn(o pnigKr BHs: Kerr spinning (for spin MBH the denotes M • sirens + map p ∆ M ihclbainpoie yGnrlRltvt,ta provide that Relativity, General by provided calibration with , e • 2 o ∆ fteMHsaeie .. fteMHmlioemmns In moments. multipole MBH the of i.e., spacetime, MBH the of − (ln ∼ a • 2 10 M with , udmna hsc ihLISA with physics Fundamental − • 4 ) , , 3 a − ∆ Ω ∆ • 5

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2 oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 aisi on opa nipratrl n edakfo ueia Relativity Numerical required. from be feedback to going and is role theory important post-Newtonian an dy- and play gravitational to non-linear waveform going the IMRI particular, is precise In namics obtain purposes. to order analysis mod- in data EMRI enough for accurate for templates be made to approximations going the of not that modeling are The sense eling LISA. the by in detectable difficult observatories, be is would ground systems MBH advanced these an future into IMBH by an detectable of inspiral be the expected would the IMBH, exist, an they into case rals the In is range evidence. have mass observational there of although 2004), claims Colbert, from several and also been (Miller masses and exist (with IMBHs BHs BHs that stellar certain supermassive of completely and ones formation MBHs The the of from IMBHs. ones different the the are to IMBHs corresponds to which these up 2008), for al., channels masses et have Mandel and can 2007 object al., massive (IMRIs), inspirals central intermediate-mass-ratio from the GWs where for to sensitive particular observatories be in These to observatories, expected detectors. are ground-based third-generation fol- for and that part generation) discussion (second in the advanced relevant observations, be EMRI also LISA can on lows contribution. focuses this article of remainder this the Although of of subject theories main alternative the of be tests oppor- to perform going unique to is a also This and provide gravity. theorem observations no-hair EMRI the LISA test to that tunity said always is it Therefore, rawiedaf ree ansqec tr.Hwvr lhuhastronomical NS, although a However, of or existence BH, star). the a of sequence be evidence main also accumulating a providing can are even (that to observations SCO or going a dwarf, are and white assum- MBH we a been a all, have or by we of composed here observations are First Until EMRIs EMRI EMRIs. that of LISA face. ing status with we theoretical do that the is to challenges what try theoretical summarize actually the can are we what what and discuss now us Let 3 h cwrshl ouin(e,eg Wl,18).TeShazcidslto a a has solution matter Schwarzschild by The the described 1984)). on BH (Wald, spherical e.g. conditions (see, a certain solution be Schwarzschild must under the collapse that Universe; spherical of early known point the end is in the it overdensities distribution, Relativity, of General collapse star; In cluster; massive star a etc. a of of collapse core Direct the form: of can collapse MBHs which in ways different are There of aspects different on accounts exhaustive physics). for particles BH 1997) (Chandrasekhar, neither Novikov, (see that infinity and sense null Frolov towards the and region in 1992 this region, from escape BH can the flat rays escape, light asymptotically no nor is of geometry region spacetime a contain whose un- and Objects we as theory: MBHs be in we must Way), them objects Milky these derstand that the galaxy, conclude to own arguments our definitive (including no have centers galactic all almost at objects hthptei ecntyt etwt EMRIs? with test to try can we hypothesis What M • ∼ 10 2 − 10 udmna hsc ihLISA with physics Fundamental 4 M

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M dark .I sntyet not is It ).

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13 oe esfrG science GW for News & Notes Notes & News for GW science 14 WNotes GW u (spin) tum ceie yol w tre xenlyosral aaees Mass parameters: observable char- externally Ein- completely (three) the be two of can only solutions Relativity, by BH General acterized all in that 1971) postulates equations, Wheeler, which (Einstein-Maxwell) and denomination, stein (Ruffini BH Wheeler the with as associated well proven), as been not has it since so-called the to leads This situations). astrophysical BHs in those quickly expect very we although discharge 1965), to al., et (Newman geometry de- spacetime fully Newman it is mass that BH is the geometry numbers, spacetime two Kerr by the termined of characteristic BHs. important of BH One 1963) stationary (Kerr, 1973 vacuum family Ellis, only Kerr the and the that by (Hawking asserts described see that those theorems; details) are Relativ- solutions for of General 1973) in series al., that a et out (actually Misner turns and theorem It that BH. a expect stationary is a should there is we ity collapse correct, the of is state conjecture final censorship the cosmic the the with that compatible Assuming is conjecture as hoop known the horizons, without that singularities In mentioning of issues). worth in appearance these issue is of key it discussion open detailed sense, the a the as this for called remains 1984) it (Wald, is of (see what proof collapse is and gravitational This formulation end satisfactory BH. the a the a hence and and But is ture horizon collapse a singularity. the by a covered of is be point singularity must this 1973)), whether sin- is Ellis, the now to and question appealing (Hawking collapse, (see nonspherical of theorems outcome gularity final the hand, other the On mass a when only and when S (Thorne, Thorne this C to relation In case. spherical the in so-called the as proposed clear 1972) as situation the means collapse, no nonspherical by exterior Regarding the is describes distributions. it matter hence spherical and all spherically equations, of vacuum field possible only Einstein’s the of is solution it symmetric as Relativity General in status special very rmti icsin hr sa biu yohssta ewn ots ymeans by test to want we that observations: hypothesis EMRI obvious LISA of an is there discussion, this From BH. the that of said field be can (they It erased away). are radiated BH are S a or horizon of the formation behind the disappear towards either evolved that fields matter the about (and adeeti charge electric (and neeydrcini one by bounded is direction every in Q r nqecnevdqatte soitdwt h xenlgravitational external the with associated quantities conserved unique are ) S • as h charge the (also Q .Alohrifrain(owa h word the what (to information other All ). udmna hsc ihLISA with physics Fundamental no-hair hoop M Q • escmatdit einwoecircumference whose region a into compacted gets ntecs fcagdBsdsrbdb h Kerr- the by described BHs charged of case the in hoe atog tsol ecle conjecture called be should it (although theorem ojcueta asta H ihhrzn form horizons with BHs that says that conjecture C < 4 π M M • . n h Hitiscaglrmomen- angular intrinsic BH the and etme ,2010 7, September naked omccensorship cosmic singularities. hair M eesto) refers n spin and conjec-

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and oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 ud Knu 91 n egadSmn(egadSmn 91 lopoe that proved infinity. also 1981) of Si- Simon, neighborhood and and (Beig the some Simon with Beig in and solutions Beig least vanish; two and at that 1981) moments (Kundu, identical case multipole Kundu static are all the moments for if multipole proved only same 1980) Simon, and asymptotically- and if and (Beig angular static, flat mon its vacuum, is all a spacetime if that only proved flat and he moreover, if static vanish; moments is spacetime vacuum, asymptotically-flat a that and by proved these stationary, later 1979) regarding and (Xanthopoulos, results Xanthopoulos spacetimes, Relevant are: static moments intro- spacetimes. of multipole stationary were case for moments the 1974) for multipole (Hansen, 1970) These Hansen (Geroch, Geroch case). by two first (actually Newtonian duced moments the multipole with of set comparison infinite vac- in an spacetime pur- by vacuum for asymptotically-flat determined our result stationary fully for similar any is used that geometry a shown be is multipole been can has there of that It Relativity set poses: spacetimes General infinite asymptotically-flat in an and that stationary, by out uum, characterized turns be It can body moments. isolated sta- gravitational different an the between theory, of distinguish Newtonian to potential In is goal geometries. the asymptotically-flat which and in tionary situation a second in are The we Then, spacetime. from vacuum enough truly isolated are a objects objects. in the massive purposes is other practical BH compare for the that we means which when assumption in negligible energy is situation these that the of density curvature with local spacetime the energy, a dark of produces sort components accelerated some whose to surrounded universe due expanding are The be an they may in geometry. expansion embedded although are flat that they these and means asymptotically matter of basically and dark geometry by assumptions vacuum exterior two a the these be that of to assume first considered also We be can precision. objects of degree whose high state a formed final were to a going objects to is these down it how settled is, of have centers independently they words, galactic other the in at or objects stationary, assume be dense to to the going of are geometry we the end, whatever that that To Astronomy). Wave Gravitational in section estimation in future other appendix the and (see in stream present geometry clear signals data Kerr is EMRI LISA the It the the from between objects practice. by discriminate collapsed in for to well hypothesis geometries method possible the described this a test at is have to objects BHs must how we collapsed these is that the of question the that geometry Now, saying the metric. is and Kerr it BHs, that are to sense centers equivalent the is galactic Relativity, in General theorem of no-hair validity the the assumes which hypothesis, This General the of solution Kerr the by described Relativity. of BHs Theory stationary are centers galactic H1: erHypothesis Kerr h ak opc n eymsieojcsstiga the at sitting objects massive very and compact dark, The : udmna hsc ihLISA with physics Fundamental WNotes GW 6 o eiwo h hoyo parameter of theory the on review a for spatial emtyi ieindependent time is geometry

15 oe esfrG science GW for News & Notes Notes & News for GW science 16 WNotes GW 2 ytm,teTon n sbsdo xasoswihaevldi pctm re- spacetime in valid are which expansions on is based geometry whose is gions one Thorne the system), hr eaeuigtemliidxntto fTon Ton,1980): (Thorne, Thorne of and )indices notation multi-index the using a are we where of type this to defines also related (which coordinates closely ACMC in systems), multipole more tensor spacetime, coordinate metric the asymptotically-flat the and and which of stationary in form any intuitive way the For the more introduced. show be to is can here moments it Thorne use we of theory, gravitational-wave approach the Since 1973)). al., et Misner by and covered 1971 be over Lifshitz, integrals can an to interior related of its are body moments and the multipole BH, Thorne a the not coordinates, Donder is coordinates). de body ACMC compact are the coordinates when Moreover, Donder/harmonic centered mass (de and coordinates Cartesian asymptotically (ACMC) namely coordinates, of type particular ieadtecnomlsrcueo h nue -ercadhsteeeac of elegance the has and 3-metric the induced on the based of is structure being it conformal space- the the one, of stationarity and geometrical the time a with associated is space three-dimensional formalism the of Hansen analysis and Geroch 1983). the (Gürsel, While Gürsel by Geroch established of was Thorne moments of the multipole those characterize the and that Hansen between GWs. moments and equivalence of multipole The the sources off of geometry. slow-motion read expansion spacetime can of multipolar one emission the expansion radiation of this From case gravitational asymptotically-flat special the and a for (Thorne, is stationary, Thorne expansion Thorne a theory, This of gravitational-wave metric. expansion of spacetime multipolar context a the introduced in 1980) hand, other the On axisymmet- are moments multipole stationary its a all if that only showed ric. and 1983) as- if stationary, (Gürsel, axisymmetric a Gürsel is of spacetime metric. structure local vacuum the flat, determine ymptotically uniquely moments multipole the euetenotation: the use We 1 a 2 · · · eea covariant general a ` n ihthis with and , N g g g A effective tt ij ti ` n ≡ = = = !! ≡ n − X δ ` ∞ = a ij n { 1 1 1 t n + ( , + n a x r 2 X − i ` Q teseeg esr(hre 90 seas Lna and (Landau also (see 1980) (Thorne, tensor stress-energy ` 2 close ie tde o eyo n pca hieo coordinate of choice special any on rely not does it (i.e. } 1 ∞ · · · = udmna hsc ihLISA with physics Fundamental + )( 2) M r 0 A ( 1 i ` n n = " r + = a − ` − 1 ` + 1 oteMnosifltgoer n sepesdi a in expressed is and geometry flat Minkowski the to X 4 Q ` with 4) 1 , ∞ = ` 2 R a 2 ( · · · 1 (2 , ` a ij 3 2 r ` ; + ··· ,cnb rte as written be can ), ` 2o 1) or (2 ` n 1 − a + − ` 1)! 1 i 1 hr ssmainoe eetd(multi- repeated over summation is There . ≡ , 1)!! " (2 2 x . i  / ija r ` ` ` ( − J r ! 2 etme ,2010 7, September 1)!! jA = ` − δ 1 M N ij x A A i ` 2 x ` : + N j .I hs expressions, these In ). A R ` i ; + ` − R 1 # ` − , 1 # , A

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17 oe esfrG science GW for News & Notes Notes & News for GW science 18 WNotes GW asadcretmlioe a erltdt hs w ytefloigsimple following the next by the two these instance, to For related be them. can of relations: multipoles combination current a and is mass rest the moments, independent et eedol nteB asadsi.Ta s only is, That mo- spin. multipole and the mass all BH that the is on theorem) only no-hair depend the ments of discussion previous our from monopole mass the namely fnnvnsigmlioe sifiie hra ntennsinn ae(Schwarz- case spacetime, non-spinning static number the the in schild whereas case, infinite, general the is in multipoles that non-vanishing Note of symmetry. reflection the from expected as htis, that mo- multipole of sets two the that out turns it BH, ( Kerr Eqs. of a ments of case particular the In described purposes the for interesting article. this potentially in are they hence, and the as equilibrium interpreted been have moments These axisymmetric geometry. for et moments (Ashtekar multipole collaborators and and horizons mass Ashtekar introduced Finally, have 2004) moments. knowledge al., multipole the from of spacetime set a reconstruct the to of principle in used be also can method cuaywt hc h anER aaees(asrtoadMHms and mass MBH and ratio the of (mass estimates parameters MBH) EMRI the main of plane the equatorial which the first with in a orbits accuracy have as circular we of seen sequence Here, be a can how. is which and 1996), hypothesis practice the (Poisson, attacking in Poisson at this attempt by do work can previous we mention whether to is now question The whose Relativity of Theory vacuum, the General by the moments described multipole of well solutions be can axisymmetric centers and galactic stationary, the at sitting objects massive H1’: hypoth- our change can we observations: moments, multipole on discussion esis this all after Then, H1 erHypothesis Kerr M yaohrsmlroeta smr mnbet etse yLS EMRI LISA by tested be to amenable more is that one similar another by hc rvd ifoopimivratcaatrzto ftehorizon the of characterization invariant diffeomorphism a provide which , 2 ` = ( 4 − aif h olwn lgn relation: elegant following the satisfy ) 1) ` M { M h xeirgaiainlfil ftedr,cmatadvery and compact dark, the of field gravitational exterior The : • a ` • 2 , a ` J udmna hsc ihLISA with physics Fundamental • ` and } )teol o-aihn utpl stefis one, first the is multipole non-vanishing only the 0) = ` = M 0 ,..., 0 J M − − 2 ∞ = ` M M + ` aif h errltoso q ( Eq. of relations Kerr the satisfy 1 + M • • H1 a a = iJ • 2 • 3 • h eakbefaue(lhuhexpected (although feature remarkable The . ` hr sn ipie oe teinspiral (the model simplified a using where , ( = = − = M J 1) 3 M 2 = ` M = • M • ( M − ia a 2 M • 2 0 J • etme ,2010 7, September J ` 1 ) 1 2 + 0 ` . 1 n h etvns identically vanish rest the and , , , oremultipoles source M 0 and 5 ). J 1 = fBsin BHs of M isolated • a

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19 oe esfrG science GW for News & Notes Notes & News for GW science 20 WNotes GW ciiganme fmlioemmns(xldn obviously (excluding moments multipole of number a scribing (9) and (8) anomaly; mean where (13) and (11) respectively; spin MBH and where time fiducial A (1) 2004): Cutler, (6) and need (Barack we be configurations to EMRI taken t generic be For can that body. parameters massive 14 central the call as us let MBH detail, Kerr more in this at look hn h ai dai otk nER aeomtmlt oe hticue a includes parameters that source model of set template the waveform in section EMRI moments in an multipole of take appendix, number to certain the is works in idea His basic summarized (LISA). the EMRI theory an Then, estimation or multipole (LIGO) parameter the IMRI the determining an in by uses LISA emitted and GWs LIGO which the of in from accuracy work moments the pragmatical more estimate a to is is 1997a) goal (Ryan, the study Ryan’s of part second The inlerrof error mass of tional with SNR SCO an mass with an of and of object plunge case massive re- particular central his the a illustrate for into the to inspiraling that to order mention door In us the above. let open introduced sults, and hypothesis LISA the testing for of optimistic confusion con- possibility are the The computations include binaries. Ryan’s compact not galactic of does of clusions millions instance, of for foreground the that, by noise generated noise LISA the for model plified mati h eut o h siae cuais nodrt opt h Fisher the compute section to order in In appendix (see accuracies. an matrices estimated have variance-covariance the which and and for size, results favor characteristic the to a in try of impact which bodies analysis, compact the for in appropriate considered moments models are multipole ingredient the important Another for priors considered. the are the waveforms reduces the only (this in to of described multipole system here each description EMRI work his generic the in a of used part of first meters model model the equatorial of waveform and phase The circular GW the the modeling. essentially EMRI is the Ryan in of included moments multipole of ber form: the of θ series time be to going alteeparameters these call ayis racy finds Ryan a ie stescn ato ynswr.Teeaesvrldfeecs otof most differences, several are There work. Ryan’s simi- of in part study second an the conducted as 2007) Cutler, lines and lar (Barack Cutler and Barack Recently, with errors the of stabilization a to tendency a increasing although analysis, the in considered o I (2) ; = γ ˜ o θ where , K I ln ∆ L D ˆ for ( m and M θ stedsac otesuc.Te,w edt d xr aaeesde- parameters extra add to need we Then, source. the to distance the is K ? N 2 I ∆ (3) ; / and mm = ( M γ S ˜ S ˆ ( ∆ 1 / • t 3 sobserved. is M , . . . , ) ) M r ntvcosi h ieto fteobtlaglrmomentum angular orbital the of direction the in vectors unit are ln φ steprcne nl nteobtlpae (7) plane; orbital the in angle pericenter the is ∼ 2 / K ) M M 0 oa n zmta nlso h B pn (14) spin; MBH the of angles azimuthal and polar , ∼ 14 . • 5 θ ~ ∼ (4) ; hs roscag ihtenme fmlioemoments multipole of number the with change errors These . 10 and , M 10 nti a,temdldsgasi h IAdtco are detector LISA the in signals modeled the way, this In . − udmna hsc ihLISA with physics Fundamental 3 − θ n nlyfrtems uduoemmn h accu- the moment quadrupole mass the for finally and , S 3 S • θ 10 , / and m I M ti on htLS ol measure could LISA that found is it , = ? • 2 α θ (5) ; ihfatoa error fractional with φ o M I where , S k oaino h ore (10) source; the of location sky , h for θ ~ e ( K o t ; I = oteprmtr fERscnitn fa of consisting EMRIs of parameters the to θ ~ 7 = ) e .Te,ol h edn re fet of effects order leading the only Then, ). hr h parameters the where , ( α 15 t ( o t ) , . . . , ) h cetiiya h dca time; fiducial the at eccentricity the , steaiuhldrcinof direction azimuthal the is etme ,2010 7, September M 14 = + 10 ∆ N m 5 mm M ? /

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21 oe esfrG science GW for News & Notes Notes & News for GW science 22 WNotes GW hmfo h on fve fti ril nohrt uete u rt confirm to or out them rule to other in study article and to this interesting based of still be view is may of it models point community, these the the from in of them originate some may which they in skepticism grounds the independently weak case, possibly any the In of assumptions. topological/geometrical some by the formed circumvent are energy-momentum they that the of means satisfy which form not theorems, these do in models assumed conditions non-BH their of these several or Normally, one satisfying not premises. Relativ- by General theorems of these mod- solutions circumvent BH propose models Kerr These to the ity. room from different still field is gravitational for- there the the horizons, for els and BH in by collapse theorems covered well-known gravitational singularities the the of of of mation despite outcome that the fact regarding the Relativity on General relies this for justification A ftepeiinta IAi xetdt civ.Te,i em loraoal,for hypothesis reasonable, the also test seems can it terms we Then, in that prospects achieve. price to good same expected with the is task LISA realistic that a galactic precision seems at the it via of sitting that objects use conclude massive its can the and we of dynamics, centers, geometry EMRI the for testing for importance observations its LISA objects, geometry compact describe the that of solutions with exterior vacuum associated the and structure flat multipolar asymptotically axisymmetric, the stationary, on of discussion this all After 2005). the Apostolatos, of and fields (Sotiriou electromagnetic in possible done include was to source Ryan of reach work required. to be the order would of effects in Generalization those Thus, including only analysis extended based effects. an reaction was conclusions definite radiation analysis including their without However, geodesics, Kerr parameters. on a and orbital metric different non-Kerr with specific be may the metric there of that waveforms out between pointed the problem also in confusion and changes a detect the to from difficult induced be may Kerr or- moments from geodesic multipole deviations their the that analyzed concluded have They and Thorne, bits. geometries and non-Kerr Hartle using and constructed 2006), 1967 have Babak, (Hartle, 1968), and geometry 2010). rotating (Glampedakis (Vigeland, Hartle-Thorne Babak exterior presented and the been Glampedakis has work, BHs related compute a bumpy to In these method of a recently, moments More intro- multipole to BHs). the second, Kerr and, (bumpy construction momentum Hughes angular and duce Collins the of problems mentioned r fRltvt hs utpl moments relations: of multipole whose vac- the Relativity by The- of described General ory the well of be solutions can asymptotically-flat and centers axisymmetric, galactic stationary, uum, the at sitting objects massive very H2: hypothesis: general more -oyHypothesis X-Body exotic R a [ atr(upre ysm xtcpyis.I sas osbeto possible also is It physics). exotic some by (supported matter { M ` , J ` } ] h xeirgaiainlfil ftedr,cmatand compact dark, the of field gravitational exterior The : = udmna hsc ihLISA with physics Fundamental 0 ( a = 1 . . . , ). { M H1’ ` etme ,2010 7, September , J opromtsso h following the of tests perform to , ` } ` = 0 ,...,

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23 oe esfrG science GW for News & Notes Notes & News for GW science 24 WNotes GW ftepyia aaees(e pedxi section how in of estimation appendix the question (see perform the parameters to is models physical waveform essentially the necessary the and of the get question produce we practical to once going program a this we we is out are that This carry question to important going data? an we LISA are still real How is of solve: there discussion and now, face the until to all done have from been has come that that work prospects the good the despite and Nevertheless, (Johannsen spectrum electromagnetic the 2010b). the of 2010a, tests in Finally, Psaltis, proposed and 2010b). re- 2010a, been 2008b, discussed have (Brink, been theorem papers have of problem no-hair series EMRI a integrability the in to the Brink impact by to the cently related and questions orbits Other geodesic the distinguished observations. be of EMRI may that LISA geometry GW future non-Kerr the a the of of in evolution fingerprint a the as during seen frequencies be of can ratio signal the of constancy This quencies. 1 r omnual terrtoi ainlnme)dsnert oa ofr a form to as so disintegrate number) so-called rational the a of is chain ratio three) (their the or inte- commensurable them Kerr of are the (two to frequencies per- fundamental (corresponding as associated tori seen whose space motion) solutions, phase grable Manko-Novikov the the solution, Lukes- in Kerr that the Apostolatos, of shown turbations was by Lukes-Gerakopoulos it extended where and 2010), 2009 was al., al., work et et This (Apostolatos signa- Contopoulos observable and waveforms. Gerakopoulos induce EMRI may mo- the behavior orbital of in chaotic the integrability This tures with of associated behavior. lost space space- chaotic the phase of exhibit the class to tion this of due of regions quadru- that, configurations certain mass is certain geometries, the from study time come at this that already of equations starting outcomes geodesic the the solution multi- of Kerr One whose the 1992), of pole. those Novikov, from and differ (Manko poles solution Manko-Novikov the namely ac,i sblee httecretost h edscobtlmto hudbe the should point motion some at rele- orbital and of time geodesic in ratios the up mass build to corrections the corrections these of Nevertheless, the small. smallness that locally the believed given is and it modeled, vance, are EMRIs which in of phase GW than the smaller precise be in very should error signals require true the will the that to it estimated respect and with been templates task has these difficult It a below templates. be magnitude the waveform estimate of to GW and order going signals an is these extract about parameters have to least, physical sources, that we at different means once This of be, noise. since number to instrumental point a expected LISA’s from are crucial signals signals a GW EMRI is containing the This stream, data before. LISA listed the have we hypothesis ent ln nodrt ics h hlegsta efc nodrt ei oiinto position a in be to order mod- in the face of we ingredients that main hypothesis challenges the the the EMRI are test discuss of what to status recall order present to in want and eling just basics we the Here, above wave- commented EMRI modeling. of already modeling have the We for challenge forms. theoretical considerable a supposes this er ie htsc aeomcncnano h re of order the of contain can waveform a such that Given year. H1’ ikofislands Birkhoff and udmna hsc ihLISA with physics Fundamental H2 nteprubtv eea-eaiitcframework general-relativistic perturbative the In . hr l rissaetesm ai ffre- of ratio same the share orbits all where , etme ,2010 7, September 6 eesr ots h differ- the test to necessary ) 10 5 ylso more, or cycles

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25 oe esfrG science GW for News & Notes Notes & News for GW science 26 WNotes GW r on ob rsn npyial elsi ae.I te od,prasnot perhaps words, other In moments all multipole exhibit at cases. the literature clear realistic the of not physically in combinations is in studied possible it present cases all since be the BHs, to of some going bumpy that are of features study particular provide the can the for This that about structure. guidance learn their valuable topol- and to it very spacetime interesting of a the result very would in be that more Rela- geometries would pathologies get possible General it or the to specially in matter useful allowed), collapse exotic very are where gravitational be ogy/geometry cases the some would for are of it There (even outcomes instance, tivity possible problem. For the the of into follow. we view insight can Nevertheless, pessimistic one a task. here that difficult advocate avenues quite to a want be not may do EMRI spacetimes the Relativity, non-Kerr General within to extending, that modeling not see class. can is D we it discussion type this Petrov know From the perturbative we in certainly the not are geometries, of that other geometries decoupling in in this happen happen to Again, to going BH. not likely Kerr information is a gauge-invariant equations the of all perturbation describes the that basis), about variable, complex complex a single in a tensor for Weyl terms equation in by complex equations first single perturbative found Petrov a the was the of decouple it of to as summary 1973), possible, exhaustive 1972, makes (Teukolsky, an Teukolsky tensor) for curvature is Weyl 2003) (it the al., tensor of et curvature classification (Stephani ex- Kerr see the this already Moreover, D; of has structure type above. it special Petrov mentioned as the ten- been with geometries Killing has together other symmetry, 2-rank and for tra authors a change several of to by existence likely found very the been is with This associated symmetry. is sor which 1968 (Carter, 1968), separated as Carter, completely integrable be and completely can are equation have motion Hamilton-Jacobi we cer- associated as of has the Indeed, equations it geodesic take that equations. the these sense to of the mentioned, have simplifications in already we to geometry lead respect, Kerr that this the symmetries of In tain character special dif- motion. the to orbital account also geodesic into and the equations changes for perturbative of equations different number ferent a to implies lead (i) geometries in- Point different equivalent object). since (or compact moments central multipole the include about to formation space parameter the extend To (ii) ein olt otnetewr ntesuyo h ro siainfrmultipoles for estimation error the of study the con- on ACMC a work are the the they of continue Therefore, to use 2010)). tool the Yunes, venient and (here (Sopuerta moments connected help multipole be can the systems can less with coordinate that are way approximations simple waveforms to relatively these a related produce in are 2007). to they 2004, sometimes Cutler, algorithms and and computational complex (Barack the Cutler improve sense, and and this confirm Barack can ob- In by we can given way we already this waveforms estimates in EMRI benefits and the better estimates, of produce error we types parameter as two better First, are tain advance There research. to of is waveforms. line kludge possibility this from of Another restric- development certain realistic. the only physically in that are further possible moments be of may classes it tive instead, objects, collapsed of moments udmna hsc ihLISA with physics Fundamental etme ,2010 7, September { M ` , J Ψ `

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27 oe esfrG science GW for News & Notes Notes & News for GW science 28 WNotes GW utpl oet,a hyaei eea eaiiy r o nuht determine to enough not are Relativity, the General that in be are may of they it as but lines defined, moments, the consistently multipole be in can hypothesis moments translation multipole an straightforward that of an required tests make make to to possible possible be not charges may hypothesis it col- (e.g. after of case, hair theo- produced) are that extra of numbers objects case confer In whatever two the can (or just BHs be lapse. fields the may by these to This fields) characterized which these mass). in not with the associated and is just fields, it less, extra that (or with be more ries by may but it spin) theorem, case, and uniqueness that (mass of how- in (existence be, role But may similar There alternative a solution. etc.). In plays a BH. that be Kerr solution even different a not a form may ever, should metric Kerr it system the collapse gravity, self-gravitating the of of a theories stages once all that through Gen- indications in gone strong seen, has have is very we aspect are As important there collapse. very Relativity gravitational a of eral sense, outcome this final the- In the the of question. change question into we the the put when should in that we that but gravity dynamics granted, of their for ory give and in we EMRIs take Relativity gravity of to General of have aspects of we several theory context Then, are a studied. there have and that defined we account properly that into be assume can system to EMRI going an are which we discussion, this After limit. certain a in theory fundamental more a from o upsdt ok sfrisac a apnwith the are happen can they in where instance valid regimes for other as are in work, that not to theories but supposed interested not eliminate are whether can we which we determine in because regimes to physical also studied and sufficiently be- satisfied, part been are in has they stringent, Relativity too be General might only however, Physics cause criteria, Fundamental additional to These links solutions, etc. and the theories, well-defined of as a stability such of action, ones, existence relativistic additional the complete impose formulation, can initial-value we the criteria to of these comparable well-posedness from are Apart speeds light. and of strong speed is the sector gravity dynamical where the fields, in gravitational Relativity strong General of from deviate must It regime: strong-field ihacrc h yaiso h oa ytm ii tms be must It a (iii) to describes system. that Solar existence limit the the of Newtonian dynamics the implies the as This accuracy such way high solutions, a Gen- passed. physical such to are of in reduce stability tests velocities, must and observational small It for and regime: and experimental weak-field fields that the gravitational al., weak in symmetric for et consistent Relativity a (Misner be be eral by e.g. must must described (see, It principle is It (ii) weak-equivalence field (i) 1973)). the gravitational satisfies following: the that the tensor i.e. satisfy gravity, metric that of theory theories and (Yunes metric consider One in a to observations ob- criteria. GW GW is such of with context establish 2009a) test the to Pretorius, in to can ways proposed we need many been gravity has we are that of There Hence, possibility theories systems. which BHs. EMRI decide like of to servations objects criteria can- of can way set they consistent that a a happen have can in it accommodate and even situations physical not certain to tailored are they H1 oteatraieter fgaiy sa lentv,i a be may it alternative, an As gravity. of theory alternative the to udmna hsc ihLISA with physics Fundamental etme ,2010 7, September effective H1 0 and hoista derive that theories inconsistent H2 o hs tis it this, For .

nthe in oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 I h ak opc n eymsieojcsstiga h aatccnescnbe moments relations: can of multipole solutions set centers whose following asymptotically-flat galactic Theory and the Y-Gravity axisymmetric, at the stationary, sitting of the objects by massive described very well and compact dark, the H3: LISA use to try can we kind: case, following a the such of hypothesis In test objects. to collapsed observations the EMRI say of states freedom, final of the cally fields/degrees extra with associated (where ( numbers Eqs. of in sets 1980) extra (Thorne, ex- Thorne multipolar of of since powers expansions Nevertheless, in expansions essentially properties. are their which where to pansions, cases contribute the in may specially fields objects, collapsed extra massive the of geometry the uniquely fdfeetntr htaei rnil nnw o vni ehv prediction a have we if even (or unknown principle in are that nature be different may specific parameters of the These with consideration. associated under parameters gravity account of discus- into using theory previous taken by the also itself in have gravity implicit of we already where theory a the sion, is test this to However, trying observations. of EMRI is of LISA think can we thing next The multi- of gravity. types of extra theory also the to object, related orbital massive parameters the extra central finally, describe the and to poles, of necessary properties are the that and parameters motion extra contains which quired, be: h osbeplrzto tts.Scn,te ilcnanetaprmtr,s we form so to of parameters, respect models extra with waveforms contain theories will facing gravitational they will Second, of (Eard- classification states). (see a polarization for possible Relativity be the 1973a) may General to waveforms 1973b, with the going al., compared First, et pa- are as ley ways. the consider states two in to in polarization errors complex have more more estimating we contain be of that can view They models of complex. waveform more point the the for that from difficulty is Another also rameters, and the case. analysis And Relativistic data General regime. schemes the the perturbative around strong-field by expansions the principle, weak- in make in the described, that difference be in cannot a that regime make this theory in can behaviour the to tiny gravitational to want look the modifications we of regime that sector Then, field field is strong difficult consideration. the things under probe that the makes theory EMRIs open What like we systems when gravity. with face of deal may theories we other that cases to of door variety the illustrates discussion This = 15 θ -oyi -rvt hoyHypothesis Theory Y-Gravity in X-Body I + = A N θ aestepsil ifrn es,i uhawyta hydsrb univo- describe they that way a such in sets), different possible the labels mm K I for , . . . , I 14 = + 1 , . . . , N mm udmna hsc ihLISA with physics Fundamental R 14 + a , [ N { θ M XY I ` = , where , J ` θ , M M I WNotes GW ` A for h } ( ] N t ; = I XY θ ~ ) = 0 hr h parameters the where , stenme fetaprmtrre- parameter extra of number the is h xeirgaiainlfil of field gravitational exterior The : 3 15 ] r ieyt xs ihpossibly with exist to likely are )], ( a , . . . , = 1 . . . , { M 14 1 ` ). / , + r J ` N a ecnsefo the from see can we [as , M mm ` A and , opigconstants coupling } ` A = = 0 1 ,..., ,... θ θ ∞ ~ I = aif the satisfy = ( θ θ I XY I ) {M will for ` A }

29 oe esfrG science GW for News & Notes Notes & News for GW science 30 WNotes GW where hoy h cincnb rte stefloigsmo terms: of sum following the 4D as this In written be cosmology). can inflationary to action (Wein- approach the (see theory, this action of application the an to for terms 2008) high-curvature berg, of inclusion theory the field effective through More an standpoint, from 2009). motivated Taveras, also and (Taveras is Mercuri correction invariant and Pontryagin Nieh-Yan the 2009 generically, the Mercuri, to and coupled Calcagni Barbero-Immirzi 2008, field Yunes, the scalar and 2006). when a gravity Gates, to quantum promoted and loop is (Alexander in parameter sector naturally non-perturbative arises the also term in This appear can also 1998), string it (Polchinski, mechanism perturbative but anomaly-canceling of Green-Schwarz the compactifications to four-dimensional due ap- theory in gravity quantum appears several parity It by a motivated well- proaches. represents is the inclusion term of of its new addition and generalization This interaction, a the violating is in term. that consists Chern-Simons Lagrangian modification three-dimensional Einstein-Hilbert Jackiw main known the by Their to initiated term Chern- 2003). was new Pi, Relativity Dynamical a recent and General a as (Jackiw of for Pi modifications gravity 2009) and of Yunes, of type and This theory (Alexander see review). alternative (DCSMG; particular Gravity Modified this Simons to refer We particular a in EMRIs of study gravity. the an in of of said, theory example been doing an alternative has present avoid what for we To of article part plan discussion. this illustrating speculative of clear of remainder too aim a the also with and draw and vague point to too that reaching a order in hypothesis in up of end little context may too the argument possible know in of spectrum science we the EMRI and that LISA is vast this too all from is extract cases can one that conclusion clear A find may parameters. in One physical problems the confusion high. of or identification too parameters, the is among number theory) degeneracies total the possible of the with theory with alternative if problems associated an ones view in the of system (including EMRI point an gravity practical characterize the to may necessary from this the parameters However, task estimate of testing difficult to gravity. of reduced quite of be purposes a theory can alternative the become this the for said, characterize just unknown that have as we parameters them what Following consider theory). always the can we them, for an h otygndensity Pontryagin the tains where S R EH stesaa uvtr.Tescn term, second The curvature. scalar the is steEnti-ibr action Einstein-Hilbert the is S EH udmna hsc ihLISA with physics Fundamental = S S κ = ∗ R R CS Z S = EH : d 4 α 4 x + Z p S − CS d g 4 + x R p S κ , − φ g + etme ,2010 7, September φ S H3 S matter ∗ R R = CS hn otnigti ieof line this continuing Then, . stemdfiainta con- that modification the is , 16 , 1 π G ,

(10) (8) (9) oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 lohv h otiuint h cino h clrfield: scalar the of action the to contribution the have also a field, density, scalar Pontryagin a by the multiplied φ that is spacetime, mention four-dimensional a to in important invariant topological is It respectively. tensors ture Here where  oriaesse) sgvnb se(ue n rtru,20b o h derivation): the this for on 2009b) details Pretorius, for and (Yunes 1997) (see Novikov, by given and is Frolov system), and coordinate 1992 Chandrasekhar, 1973, al., coordinates et Boyer-Lindquist-type DC- in dynamical gravity, in MBH modified rotating SMG a of field gravitational axisymmetric and stationary h cwrshl erc.Uigsalculn [ ( by small-coupling Eqs. longer described see no Using still are are They metric). MBHs non-spinnning theory. Schwarzschild is (although this the metric point in Kerr first MBHs the The spinning by of DC- described 2010). geometry in Sopuerta, the EMRIs and of of Yunes study question and the the 2009 on Yunes, far and so (Sopuerta obtained SMG results main the summarize now We of example an is fields. Finally, theory matter EMRIs. the study of non-spinning cannot version we of this where is Hence, theory perturbations gradient 2008). forbids whose Sopuerta, and and fields dis- (Yunes 2008) scalar BHs it Yunes, for particular, and solutions In the (Grumiller BH constraint, restrictive. spinning time-like additional too of an is to possibility leads which the density, this allows that Pontryagin out the turns of It vanishing action). the to tribution field o h CM clrfield scalar DCSMG the for for relations where oie erc si h aeo h ermti,rmiscmltl determined completely remains mass metric, the Kerr numbers: the two of only case by the in as metric, modified where nGnrlRltvt.Hwvr h utpl oet ontstsyterelation the satisfy metric Kerr not the do ( with Eq. moments as in multipole theory, given the this However, in metric Relativity. this General for in theorem no-hair a establish to µνρσ opoueamdfiaino h eea eaiitcfil qain.Te,we Then, equations. field Relativistic General the of modification a produce to , φ and α g β ds a ocdt eafie ucin(ihu yaisadhnewt ocon- no with hence and dynamics (without function fixed a be to forced was ∗ R R steculn osatascae ihtePnrai est em and term, density Pontryagin the with associated constant coupling the is µν saohrculn osat nteoiia eso fteter,tescalar the theory, the of version original the In constant. coupling another is Kerr 2 10 dx R = n ( and ) µνρσ µ ` steln lmn o h ermti.Temlioa tutr fthe of structure multipolar The metric. Kerr the for element line the is dx 5 R o all for ) ≥ µνρσ ν r h pctm eiCvt niymti n imn curva- Riemann and antisymmetric Levi-Civita spacetime the are 4 = S hc nov h parameter the involve which , 11 ds φ ∗ R ]adso-oain( slow-rotation and )] = 2 µνρσ ` = φ − tcnb enta h utpl oet aif different satisfy moments multipole the that seen be can It . β ds = = udmna hsc ihLISA with physics Fundamental Z Kerr 2 5 8 φ 2 1  d α β is: µνρσ 4 + M x a • 5 p • M R 4 ξ cos( − r µνγδ • 4 a g r • n pnparameter spin and 2  θ " R 1 2 1 WNotes GW ) γδ g +

a ρσ µν 1 • 12 + . /  M 7 ∇ M r 2 S µ • M r • φ matter  ξ   + nteohrhn,tesolution the hand, other the On . + ∇ ξ/ 1 27 10 18 prxmtos h exterior, the approximations, ) ν steato fayadditional any of action the is 5 M φ M r M r  2 2 • 4 • 2 + • 2 # a  ! sin • V hrfr,w a try can we Therefore, . , ( 1 { φ 2 t where , , ) θ  r ,φ θ, , td dt , , ϕ } ξ se(Misner (see ≡ α 2 / ( βκ (11) (13) (12) ) ;

31 oe esfrG science GW for News & Notes Notes & News for GW science 32 WNotes GW utplrepnin(hre 90.Ti ehdo optn MIwaveforms EMRI computing GW of the method using This computed 1980). are (Thorne, waveforms po- expansion the Lienard-Wiechert multipolar 2009) Yunes, gravitational and the 1981), (Sopuerta in Sasaki, using in propagate and computed tentials, (Ruffini to are with assumed waveforms contrast are the In emitted where geometry. GWs background and spacetime geodesic flat be a to assumed is motion MBH the that assuming by DCSMG ( in Eq. EMRIs by about described think well is can geometry we point like this DCSMG, can At in studies metric future a that expect questions. such We these of on etc. role light conditions, this some the some shed in on under MBHs studies unique spinning ( is yet for Eq. it solution no of whether exact solution is an MBH there yet the Thus, no that is theory. remark There to one. want approximate we an point, Pre- is and this (Yunes At geometry MBH 2009b). the by torius, determined fully and axisymmetric is which CM oei Spet n ue,20)wscridoti h prto h so- the of spirit the in out carried was 2009) in Yunes, EMRIs called of and dynamics (Sopuerta the on in of study analysis done related the a DCSMG Then, for DCSMG). to 2010) in distance al., GWs et with of (Garfinkle propagation fast mode, (see the too zone breathing decays radiation but a the dynamics in mode, strong-field observable be additional the in an impact is an there polarizations has same that although two Relativity, the perceive General ob- only that in can 2009) Yunes, sources as and GW (Sopuerta the shown from af- been away is has far propagation it servers and all, of emission First GW DCSMG. how in is fected address to question important next The in motion orbital geodesic for take acts they correction values the Kerr. DCSMG to respect the with that change motion Notice geodesics of counter-rotating rotation). and spin co- MBH against to the to correspond respect signs (with (lower) upper the where 2009b): Pretorius, and (Yunes follows as ISCO Kerr or- the circular to innermost-stable respect the with of shifted location is the bit modified that the see Analyzing can can 2009). one Yunes, geometry equations, and Kerr geodesic (Sopuerta the function in single a equations equations in the the encoded to Once be respect Kerr. with of difference case consequence, the the a sta- in separated, As as are also tensor. integrable is fully Killing it are 2-rank equations a (i.e. geodesic has the metric also Kerr and the axisymmetric), as and ( symmetries tionary Eq. Killing in Relativity. same given General the metric has in the proximation, as that theory, out 2009) this Yunes, turns and in it (Sopuerta orbits Moreover, shown geodesics been has follow It point-particles MBH. that the around SCO the of motion semi-relativistic h pnefcs n a locekta h he udmna frequencies fundamental three the that check also can One effects. spin the R ISCO = | 6 M ∓ prxmto Rfn n aai 91,weeteorbital the where 1981), Sasaki, and (Ruffini approximation erISCO Kerr 4 √ udmna hsc ihLISA with physics Fundamental 3 6 {z a • − 18 7 12 a M • 2 .Te,w aet oka h qain of equations the at look to have we Then, ). • } ± CM Modification DCSMG etme ,2010 7, September | 77 5184 12 √ 6 ,u otesm ee fap- of level same the to up ), {z a • βκ α M 2 • 4 } ,

(14) 12

) oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 n htalteesmlrte ilsriei eprsuiso hster,i sthe is it theory, this of type studies the deeper of hypothesis in where survive theory will Assum- of type similarities expansion. in these multipolar approximation different all same but of that the metric essentially level ing Kerr has the metric the at MBH as The least structure Relativity studied. at geometric been General EMRIs, has with case of DCSMG similarities dynamics the some which the are to there refers DCSMG what in in that seen have We pulsar. double the from one to the likely than are stringent constraints more these be and constraints, better produce can observations range IMRI the the in of observations masses from total obtained 2009b): be Pretorius, can and (Yunes that pulsar constraint double the with compared be to is which to es- accuracy This the broken). of as: be expressed can be above can mentioned orbital degeneracy timate same the waveforms the that (assuming comparing also DCSMG esti- and by in could parameters computed given rough gravity waveforms was a with DCSMG GR observations which analysis, in EMRI to computed the LISA accuracy in via the constrained effects of be 2009) reaction Yunes, radiation and including (Sopuerta mate not of spite In dynamics. field EMRI scalar the reaction DCSMG in in the radiation away ex- obtained of the presence one has to the the DCSMG to contributions as due in subdominant mechanism waveform) found are metric There one the the Relativity. on that General (dependence form out same turns Isaacson the (the it actly GWs and the 1968b)), approximation for tensor (Isaacson, short-wave energy-momentum tensor the with effective in unchanged an specifically, are introduce formulae can More emission we Relativity. GW the the General using order to leading by respect to 2009) that Yunes, found this and was of It (Sopuerta examination in first out a carried effects, short-wave was reaction radiation DCSMG of in importance question the of view In degener- this included. break be to to order need In effects DCSMG reaction waveforms. in radiation Relativistic parameters acy General orbital the find match always can can that a we Given cor- parameters, way: and different orbital frequencies a fundamental responding in associated seen its be with waveform can Relativistic This fun- General General versa. of vice in set and parameters the DCSMG, given orbital to and of a only Relativity sets that different due imply to is differences corresponds Relativity These frequencies General damental geometry. of MBH framework the the in waveforms in differences these computed between dephasing ones the the and and effects so-called reaction the produce radiation to contain Kerr not for 2007) al., et (Babak kludge in merical used one the to similar is h rsmbeB tSrA Sgr Moreover, at BH etc. presumable orbit, the of type the SNR, the prxmto Iaco,16a 98)(e lo(inre l,1973)). al., et (Misner also (see 1968b) 1968a, (Isaacson, approximation aeom.TeDSGER aeom bandi hswydo way this in obtained waveforms EMRI DCSMG The waveforms. ξ udmna hsc ihLISA with physics Fundamental a emaue,wihdpnso h nerto time, integration the on depends which measured, be can 10 ∗ ξ 3 norMlyWy ae obe to taken Way, Milky our in 1 / − 4 10 . 4 5 M · 10

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33 oe esfrG science GW for News & Notes Notes & News for GW science 34 WNotes GW IAcndsigihbtenGnrlRltvt n DCSMG. well and how Relativity see radi- General to of between analysis role distinguish estimation the can parameter analyze LISA perform to to important and specially knowledge effects is deeper reaction it a ation get sense, to this need In we better subjects. it understand several within to of EMRIs order of in dynamics way, the is same waveform and direction the theory this the this In in in work prospects. more parameter these but alter- confirm extra tests, to an reliable one required testing perform add to where to feasible situation seems means a it only models, in gravity Then, of hair. theory new native any introduce not does field ol nyhv netaprmtr namely parameter, extra an have only would ftedsac otesuc,a xaso htwrswl ntewa-edregime weak-field the in well works that expansion inverse an the multipole source, in the the expansion to that an distance of is (for the coefficients 2004)) the of out in pointed Hughes, appears been and that numbers has (Collins are that Hughes moments reason and possible GW Collins A the the remark by like intricate. to instance observables quite want and we be sense, moments to this multipole seems In also the phase is future. between there the relation done, in the been out that has carried fact work be of to research lot the of a and lot although tools, a seen, necessary have observa- the we EMRI develop we As LISA to Then, status. with face present we tested relations. that be of challenges can set theoretical that particular the hypothesis very tions, of of a type terms satisfy the in they discussed and determined have spin, fully the of are and BHs that mass the moments the important, multipole more have is what Relativity of by and sets General compact initiated Different objects, self-gravitating different thought moments. of to multipole of geometry corresponds their line by moments the univocally that the determined fact followed be the can have objects used we who question, others, and of Ryan type first the the For by described well is grav- BHs, the or by Relativity. stars of determined neutron Theory as like General field, objects gravitational compact whether the of Second, the of field geometries. in regime itational of And field types strong Relativity. other the test General not to of or possible solution be Kerr may galac- the it the case, by in negative objects described compact well massive is very the answer: centers of can tic geometry LISA of the that area not questions the or of us whether particular, types allow First, two in will are impact, there this make will Here, that will that Physics. way LISA Fundamental discoveries a that of scientific such source idea diverse in particular the produce a systems, support to in to these been tried of measurements has have We precise focus very The EMRIs. LISA the future. that LISA, the band for in low-frequency GWs out the have carry in to we observations expected the all, is of and of Astronomy, Wave importance First Gravitational the of it, area presented. emergent within the been perspective EMRIs has in of put Physics observations to Fundamental future tried that for possibilities offer the LISA of view by personal a article this In 4 ( Eq. of metric approximate eak,Cnlsos n rset o h Future the for Prospects and Conclusions, Remarks, udmna hsc ihLISA with physics Fundamental 12 nydpn ntems,si,and spin, mass, the on depend only ) ξ etme ,2010 7, September stemlioemmnso the of moments multipole the as ,

ξ h scalar The . oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 lse ftere.I sas a fmkn rgesi h oegnrlae of area general more the in progress making of different from way expect a can also we Physics. is what Gravitational into It insight some theories. get of Relativity, to classes General starting of of way modifications good Chern-Simons a cases, about is particular here studying described that with one view objects of the the here state the as advocate our study to and like situation and would complex gravity we this knowledge, problem. Given of coupled there. theory field a it the gravitational is regard, strongest mas- fix EMRIs the this of with always geometry In gravity can the of we testing theory theories. Nevertheless, of the other problem and in know the objects EMRIs we general, collapsed of sive in Therefore, that, dynamics Relativity. mentioning the General worth of have is as gravity priori detail of a theories great little few same that very the fact the ob- in EMRI to studied LISA due of been partly means is by test situation general to This expect in can predict given servations. we to that phenomena complicated physical seen quite of is have kind it what we available, gravity, theories of of spectrum theories wide the alternative of tests regarding we Finally, what is exhibit to Universe. them the and of in literature some see the that to in behavior expect new studied can the been not have or that whether objects understand non-Kerr some are of chaotic illustrative examples or the realistic the qualitatively how radi- of know change these to can is important they question how important whether Another know and picture. to be then can is effects question reaction interesting parts ation (observable) An initial stronger the inspiral. are in the than effects smaller of radiation-reaction significantly the time-scale massive a where central in region operate the and the of the precisely near region is only strong-field occur This the can in body. behavior and chaotic orbit that circular found the mo- stable been ergodic/chaotic of innermost has of it integrability cases, possibility of many the In question and tion. the spacetimes, non-Kerr is in arisen orbits has geodesic that question important Another and directly more models. waveform be the should to but related moments clearly multipole provide deep the should the alternatives to try about These information we learning description. signals, equivalent multipolar of GW the field process the to strong of the alternatives features find in the the to that in and idea motion moments good multipole orbital a between the be connection whereas by may one, precisely it strong Then, affected the more region. in is not but phase regime GW strong-field the moderately the in even and 5 fEuainadSine(E)adb ai ui nentoa Reintegration CFS International Curie Ministry Marie Spanish article. a the this by of and of (MEC) Program topic Science Cajal U. and the y Schutz, Education to Ramón B. of related Poisson, the E. from discussions Lehner, support for Berti, L. acknowledges Yunes E. Jaramillo, Barceló, N. L. C. J. and Barack, Gair, Sperhake, L. J. Babak, Drasco, S. S. Amaro-Seoane, Canizares, P. P. thank to like would We Acknowledgments udmna hsc ihLISA with physics Fundamental WNotes GW

35 oe esfrG science GW for News & Notes Notes & News for GW science 36 WNotes GW ihteFuirtasomo h inl,wihw eoewt id n s the use and tilde a with denote definition its we for which convention signals, following the of transform Fourier the with o IAa thssvrldfeetcanl) e ftm eista a erepre- be can that series time of set a vector channels), the different by several sented has it as LISA for wihi h ore rnfr ftenieatcreainfunction: autocorrelation noise the of transform n Fourier the is (which of set a of output the considering by start us Let that presentation has the standard. material and quite This places is different here article. in provide this we authors Esti- of other Parameter discussion many the by the presented of for been aspects relevant the of are theory of that the some theory of summarize mation aspects we general Here, for 1968) extraction). Flanagan, (We- Helstrom, signal and and and 1995) (Cutler Will, 1962 and Flanagan Zubakov, Poisson and and and 1993 instein Cutler Chernoff, and 1992), (Finn founda- (see (Finn, solid others Finn and a 1994), of given was works signals the GW in of tion measurement and detection of theory The 6 Super- de Centre the of Galicia ICTS-2009-40). de resources number Supercomputación project de the (CESGA; Centro the uses gratefully and CFS (CESCA) is Catalunya of de Spain) computació research of The Innovation and acknowledged. and Science (MEC) of ESP2007-61712 contracts (Ministry the FIS2008-06078-C03-01 from support Frame- Financial Community Programme. European work 7th the within (MIRG-CT-2007-205005/PHY) Grant etrnotation realization,vector noise the particular of a component of Fourier bility given a of probability the noise, that means which Gaussian, is and noise strumental where ojgto ya asterisk) an by conjugation is noise components instrumental Fourier different the the that assume response, we a purposes, produced noise, have instrumental that the signals into GW split be can output detector The α ( t ) pedx aiso h hoyo aaee Estima- Parameter of tion Theory the of Basics Appendix: n β n ˜ < ( α t ( + · · · f ) τ olw asinpoaiiydsrbto ucin hn h proba- the Then, function. distribution probability Gaussian a follows , ) > > t en otk h vrg vralpsil elztoso h in- the of realizations possible all over average the take to means where , n = ( n s α S α ) h αβ ( < < ) t ) ( udmna hsc ihLISA with physics Fundamental n · · · ˜ f ( α α ) ( stes-aldoesddseta est ftenoise the of density spectral one-sided so-called the is s > ˜ f = α ) t ( n ˜ en ieaeae.W loasm httenoise the that assume also We average). time means f 1 β ) , ( n ˜ 2 ≡ f α , . . . , 0 ( ) Z f ∗ −∞ ) > n + r norltd hti w eoecomplex denote (we is that uncorrelated, are o α = D ∞ a ewitna Fn,19)(euethe use (we 1992) (Finn, as written be can , .I Wter ti ovnett work to convenient is it theory GW In ). ts dt 2 1 δ h ( α α f ( ( t − t ) etme ,2010 7, September ) e i.e. , D 2 f π 0 t f i ) eetr wihi appropriate is (which detectors S stationary . n αβ s α ( ( f t ) ) , = n n α ( α hc en that means which , t ( ) t n h different the and , ) + h α ( t ) C o our For . n αβ ( τ )

(16) (15) ≡

< oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 hs fteata Wsga htpse hog h eetr is detectors signals the the through passed measuring that of signal GW actual the if Thus, signals where ie by given say noise, the of realization given a For parameters. best-fit that functions of set a by described number be a can on detector depend the in signals GWs the that sume vlae at evaluated where at evaluated meters where a hnb enta the probability the that this seen call which be we at then which can parameters maximum, the a of has values function the distribution finding by estimated be can vrrpae nie ntenx w equations) two next the in indices repeated over the on centered distribution Gaussian by a given and assume values will correct parameters by best-fit parameters the true SNR, and best-fit the between ence edfietemaueeterri h parameter the in error measurement the define We ntedtcosdt tem hn h rbblt facranvleo h parame- the of value certain is a data of detector present probability the is the given signal Then, ters a such stream. that data decide detectors to criterion the some in have we that assume also us Let ( Γ p θ ·|· p ~ ( IJ s h so-called the , ) and | eoe h ihrifrainmti,wihi endby defined is which matrix, information Fisher the denotes θ santrlinrpouto h etrsaeo inl hc,gvntwo given which, signals of space vector the on product inner natural a is ~ ) θ sthe is ~ θ ~ q = sdfie sflos(hr ssmainoe eetdindices) repeated over summation is (there follows as defined is , δθ < = θ ~ θ ~ bf priori a bf p I hn h ainecvrac arxo h errors the of matrix variance-covariance the Then, . ( ifrn elztoso h os ilgv iet different to rise give will noise the of realizations Different . p p δθ θ N ~ ( | | δθ q priors s J fsuc parameters: source of
) ace filtering matched > udmna hsc ihLISA with physics Fundamental I s = = ) ≡ spootoa to proportional is = rbblt httesga scaatrzdb h para- the by characterized is signal the that probability p Re 4 Σ ( hn h revleo h oreparameters, source the of value true the Then, . r s IJ p | θ ~ det ( + Z n exp ) Γ IJ 0 SNR O = ∞  ≡  2 n f d SNR Γ π

o  ) = ∂θ WNotes GW −  ∂ h ∝ h S 2 1 p exp − I n − 1 e N ftesignal the of SNR  (

 − 1 h s ∂θ ∂ ( 2 1 = |  − h f h ( exp h − n ) J ) ( i h o ! ( Γ αβ | 1 2 , t n ( ; − o θ , ~ n Γ θ 1 ) ~ δ − p ) ˜ ) IJ ) , θ ~ | α IJ s 1 2 with ( θ ( δθ ( n − + f s I ) ) I h ∗ − O y(hr sn summation no is (there by δθ ≡ q ( ˜ best-fit h  θ β ~ θ ~ SNR J ( | θ ) ~  n s f  = bf )  ednt h differ- the denote we , h − , . ( ( , n ssml ie by given simply is θ h − ) 1 I ) parameters )  o − h e snwas- now us Let . and . h probability the , θ ~ true I o large For . = δθ 1 I , . . . , , θ ~ Σ θ ~ bf IJ (17) (18) (21) (22) (20) (19) (23) true It . is , N . ,

37 oe esfrG science GW for News & Notes Notes & News for GW science 38 WNotes GW hc,b ento,aei h range: the in are definition, by which, ealddsuso fteueo h ihrmti nlssi h otx fGW of context the in analysis matrix Fisher the of for estimation. use 2008) (Vallisneri, parameter the See of limit. discussion SNR large detailed the a in meaningful are quantities these that n h orlto ofcetbtenteparameters the between coefficient correlation the and udmna hsc ihLISA with physics Fundamental C IJ ( ∆ θ ~ θ ) I − ≡ ≡ 1 √ √ C ≤ Σ Σ Σ II II IJ Σ IJ , ( JJ etme ,2010 7, September θ ~ ) , ≤ 1 θ ti motn oremarks to important is It . I and θ J as

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, oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 yn .D 19) feto rvttoa aito ecino oeutra orbits nonequatorial on reaction radiation gravitational of Effect (1996). D. F. Ryan, into object compact a of orbits inspiral circular the from on waves reaction Gravitational radiation (1995b). D. gravitational F. Ryan, of Effect hole. black (1995a). the D. Introducing F. Ryan, (1971). A. J. Wheeler, and R. OF TREATMENT Ruffini, SEMIRELATIVISTIC A ON (1981). M. simulator. Sasaki, LISA and The R. (2003). Ruffini, O. Poujade, and J. N. Cornish, an J., for L. Rubbo, Supernovae from Evidence Observational (1998). others and G. electromagnetic A. to approach Riess, axiomatic An (1997). M. R. Wald, the and in C. observations T. with Quinn, gravity strong-field of tests and Probes optimal LISA (2008). The D. (2002). Psaltis, W. J. Armstrong, and L. S. Larson, M., Tinto, A., T. Prince, yn .D 19b.Saa ae rdcdb clrcag riigamassive a orbiting charge scalar a by produced waves Scalar (1997b). D. massive F. a Ryan, of moments multipole the estimating of Accuracy (1997a). D. F. Ryan, hpr,S .adTuosy .A 19) omto fnkdsnuaiis The singularities: naked of Formation (1991). A. S. Teukolsky, and L. Have relativity. S. of Einstein Shapiro, century Will A (2009). (1999). I. A. I. S. Shapiro, Hughes, and C. Cutler, J., Centrella, F., B. Schutz, LISA. with physics Fundamental (2009). F. B. Schutz, stars. boson relativistic General (2003). W. E. Mielke, and E. F. Schunck, spacetime. Kerr in mechanics Celestial (2002). W. Cosmology Schmidt, and Astrophysics Physics, (2009). F. B. Schutz, and S. B. Sathyaprakash, rudaKr lc hole. black Kerr a around moments. D multipole view arbitrary with body axisymmetric massive, a hole. black spinning a around 24:30-41. 116:1009-1038. oywt rirr utpl moments. multipole arbitrary with body inspiral. binary a of waves 56:1845-1855. gravitational the from body ilto fcsi censorship. cosmic of violation . Gravity?. on Word Last the 26:094020. Gravity Quantum Gravity Waves. Gravitational with H RVTTOA AITO RMAMS HUTDIT A INTO THRUSTED HOLE. MASS BLACK A FROM RADIATION GRAVITATIONAL THE Proceedings Conference Physics of Institute Constant. Cosmological a and Universe Accelerating spacetime. curved in D particles Review of reaction radiation gravitational and spectrum. electromagnetic sensitivity. 52:5707-5718. , 19:2743. , 56:3381-3394. , hsclRve D Review Physical rgeso hoeia Physics Theoretical of Progress 20:R301-R356. , udmna hsc ihLISA with physics Fundamental hsclRve D Review Physical iigRvesi Relativity in Reviews Living iigRvesi Relativity in Reviews Living 66:122002. , hsclRve D Review Physical hsclRve Letters Review Physical WNotes GW eiw fMdr Physics Modern of Reviews 686:307-310. , hsclRve D Review Physical 53:3064-3069. , 66:1627-1638. , 52:3159-3162. , lsia n unu Gravity Quantum and Classical 12(2). , 11(9). , 66(8):994–997. , lsia n Quantum and Classical srnmclJournal Astronomical 56:7732-7739. , hsclRve D Review Physical 71:S41–S53. , hsc Today Physics lsia and Classical hsclRe- Physical American Physical , , , ,

45 oe esfrG science GW for News & Notes Notes & News for GW science 46 WNotes GW ad .M (1984). holes. M. black R. bumpy Wald, of orbits and Spacetime (2010). A. . S. holes. Hughes, black and bumpy J. of S. Vigeland, moments Multipole (2010). J. S. Vigeland, assess- the in matrix information Fisher the of abuse and Use (2008). M. Vallisneri, Relativity. General of Tests Experimental (2008). radiation. G. gravitational S. Turyshev, of expansions Multipole (1980). In S. K. Review. Thorne, Short Collapse–A Gravitational Nonspherical (1972). S. Fundamental K. I. Thorne, Hole. Black Rotating a of Perturbations (1973). A. S. Teukolsky, Grav- for Equations Wave Separable Holes: Black Rotating (1972). Field: A. Scalar S. Teukolsky, a as Parameter Barbero-Immirzi The (2008). N. Yunes, and V. Taveras, binaries. verification LISA The (2006). A. Vecchio, and A. Stroeer, (2003). E. Herlt, and C. Hoenselaers, M., MacCallum, D., Kramer, H., Stephani, (2009). A. W. P. Roming, and P. Meszaros, F., Halzen, N., Gehrels, M., Stamatikos, Timing. Pulsar with Relativity General Testing (2003). H. I. Stairs, Probe Anisotropy Microwave Wilkinson Year First (2003). others and N. mas- D. a Spergel, around geometry the Tracing (2005). A. T. Apostolatos, and P. T. Sotiriou, ebet .P .adohr 21) ttsUdt ftePre usrTmn Array. Timing Pulsar Parkes the of Update Status (2010). others and W. P. J. Verbiest, for Waveforms Approximate Improved (2010). N. Yunes, and F. C. In- Ratio Sopuerta, Intermediate-Mass and Extreme- (2009). N. Yunes, and F. C. Sopuerta, hsclRve D Review Physical prospects. D parameter-estimation gravitational-wave of ment Science Particle and Nuclear Physics Modern Freeman. H. W. Francisco. San editor, R., J. Klauder, Perturba- Neutrino-Field and tions. Electromagnetic, Gravitational, for Equations 1118. Perturbations. Electromagnetic and itational Gravity?. Quantum Loop from Inflation K- Gravity tum equations field Einstein’s of solutions Astro2010 the for Paper White A . Survey. Decadal GRBs: with Astronomy Multi-Messenger Relativity Supplement Parameters. Journal Cosmological trophysical of Determination Observations: (WMAP) mass its waves, gravitational moments. through electromagnetic measure, and moments to body axisymmetric sive, lsia n unu Gravity Quantum and Classical Scheme. Chimera The Inspirals: Extreme-Mass-Ratio Gravity. Modified Chern-Simons 80:064006. Dynamical in spirals 77:042001. , h srpyia Journal Astrophysical The 6(5). , 23:S809-S818. , eea Relativity General 52:299-339. , 81:024030. , udmna hsc ihLISA with physics Fundamental ai ihu ai:Jh rhbl Wheeler Archibald John Magic: Without Magic 58:207-248. , 148:175-194. , 27:084015. , 185:635–648. , h nvriyo hcg rs,Chicago. Press, Chicago of University The . abig nvriyPes Cambridge. Press, University Cambridge . hsclRve D Review Physical etme ,2010 7, September hsclRve D Review Physical hsclRve Letters Review Physical npreparation In 71:044005. , hsclRve D Review Physical lsia n Quan- and Classical 78:064070. , nulRve of Review Annual iigRvesin Reviews Living hsclReview Physical ae 231, pages , . eiw of Reviews 29:1114– , h As- The Exact

, oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 ue,N,Boan,A,Hge,S . oea ilr .adPn .(2010). Y. Pan, and M. Miller, Coleman A., S. Hughes, relativity. A., general Buonanno, N., in Yunes, moments Multipole Gravity. (1979). of Tests C. Precision B. Xanthopoulos, PTG-1: Letter Resource experiment. (2010). and M. relativity C. general Will, between confrontation The (2006). M. C. Will, ue,N n rtru,F 20a.FnaetlTertclBa nGravitational in Bias Theoretical Fundamental (2009a). F. Pretorius, and N. Yunes, Gravity: Modified Chern-Simons Dynamical (2009b). F. Pretorius, and N. Yunes, ue,N n oura .F 21) etn fetv unu rvt ihGrav- with Gravity Quantum Effective Testing (2010). F. C. Sopuerta, and in N. Yunes, Holes Black Schwarzschild of Perturbations (2008). F. C. Sopuerta, and N. Yunes, A experiment: and relativity general between confrontation The (1998). M. C. Will, experiment: and relativity general between confrontation The (1996). M. C. Will, (1993a). M. C. Will, (1993b). M. A C. experiment: Will, and relativity general between confrontation The (1992). M. C. Will, einstein’s to principia newton’s from gravitation Experimental (1987). M. C. Will, Thirty b1913+16: pulsar binary Relativistic (2005). H. J. Taylor, and M. J. Weisberg, Inflation. (1962). D. for V. Zubakov, and Theory A. L. Field Weinstein, Effective (2008). S. Weinberg, oeigEteeMs ai nprl ihnteEfcieOeBd Ap- Effective-One-Body the within Inspirals proach. Ratio Mass Extreme Modeling A Physics Physics of Journal Relativity in Reviews Living neSeries ence Inspirals. Extreme-Mass-Ratio from Waves itational Gravity. Modified Chern-Simons D Review ical Framework. Post-Einsteinian Parameterized the and Astrophysics Wave Approximation. 79:084043. Slow-Rotation the in Holes Black Spinning editor, Length J., L. Dixon, In update. 1998 editors, R., of J. Institute UK. Pulham, Bristol, 239–282, and Publishing. pages S. Physics Series, Graduate G. Scottish Hall, in 46 In number update. 1995 A edition. 2nd USA, York, New Books, edition. 2nd UK, Cambridge, Press, versity update. 1992 editors, W., Israel, UK. and W. Gravitation S. of Hawking, Years In relativity. general Series analysis. and observations of years NJ. Cliffs, Englewood Hall, 77:123541. 328:25. , SLAC. . hsclRve Letters Review Physical 12:1025–1028. , 228:012051. , 80:122003. , nentoa ora fMdr hsc D Physics Modern of Journal International hoyadEprmn nGaiainlPhysics Gravitational in Experiment and Theory a isenRgt:PtigGnrlRltvt oteTest the to Relativity General Putting Right?: Einstein Was . ae 017 abig nvriyPes Cambridge, Press, University Cambridge 80–127. pages , udmna hsc ihLISA with physics Fundamental 9(3). , 104:091102. , hsclRve D Review Physical WNotes GW rvt:Fo h ubeLnt otePlanck the to Length Hubble the From Gravity: srnmclSceyo h aicConference Pacific the of Society Astronomical xrcino inl rmNoise from Signals of Extraction 77:064007. , ora fPyis Confer- Physics: of Journal 1:13–68. , hsclRve D Review Physical abig Uni- Cambridge . hsclRve D Review Physical eea Relativity General he Hundred Three Prentice- . ora of Journal American Basic . Phys- , , ,

47 oe esfrG science GW for News & Notes Notes & News for GW science 48 WNotes GW Eprint: Authors: LISA Eccen- with in Orbits Binaries tric Hole Black Spinning Characterizing yais uemsiebakholes black supermassive dynamics; Keywords: Eprint: for probe dynamical Authors: a as holes S2 black intermediate-mass star Centre Galactic The universe. early the in mergers eccentricity galaxy of orbital theories the on of constraints measurements strong LISA provide can eccentricities. small from a orbits very circular in distinguish with only parts to those depends possible of it measured making accuracy eccentricity, be the an can on eccentricity to weakly the very eccentricity LISA which the typical with measure for accuracy that The to find thousand. possible we be merger, will before year it one refer- sources, the value Defining the well data. as how LISA eccentricity simulated investigate or- ence from inferred we of be effects harmonics, can parameters the higher source includes the and that precession model spin ec- eccentricity, waveform orbital parameter bital circularized. significant have seventeen already with full will band a orbits LISA the Using that the suggest enter one models that orbit will other predict while to system centricity, models begin hole evolution and galaxy black galaxy Some binary merged the the waves. of gravitational center emit cen- the and have to another galaxies sink Colliding that holes. holes black black as coalescing tral such from objects those compact of including systems sources, binary astrophysical from signals wave itational Abstract: estimation meter Keywords: http://arxiv.org/abs/1006.3563 http://arxiv.org/abs/1006.3759 e,Je hpr;Crih elJ. Neil Cornish, Shapiro; Joey Key, ulnrs lsi;Glesn tfn ert,David Merritt, Stefan; Gillessen, Alessia; Gualandris, h ae nefrmtrSaeAtna(IA sdsge odtc grav- detect to designed is (LISA) Antenna Space Interferometer Laser The sr-hC;dt nlss rq;msiebnre fbakhls para- holes; black of binaries massive gr-qc; analysis; data astro-ph.CO; sr-hG;atohsc;IR;itreit-asbakhls stellar holes; black intermediate-mass IMRI; astrophysics; astro-ph.GA; udmna hsc ihLISA with physics Fundamental eetdabstracts Selected pi oAgs 2010 August to April

etme ,2010 7, September oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 00slrmse ttedsac fteSsaswl edtcal ttenx periapse about 2018. next than in the massive at occur detectable more will be which IBH will S2, S-stars an of the that passage of degree find distance one the and the at as IBH of masses large solar an simulations as 1000 of to level presence techniques IBH a the An fitting at in shift. orbital orbit GR S-cluster observational S2’s the apply than of We larger plane even period. the or per in large as changes is induce that produce also S2 can will SBH of the apoapsis around the orbit technol- in in current shift IBH an a with be to measurable due to perturbations potentially that needs are show We (GR) effects ogy. relativity its Given and general eccentricity, star. account, large the into of taken and orbit period the orbital of short determination spectro- S2’s accurate and imaging an Near-infrared Way. allow supermassive Milky observations the the orbit scopic of to centre known the star in period (SBH) shortest hole the black (S02), S2 star of orbit the on Abstract: n iedmi ehd:Erretmts validation, estimates, optimization Error and methods: time-domain ing us- computations self-force efficient and accurate Highly < 1 at quasars at 9886 incomplete of sample highly a is on it based 1 estimates, z mass the sta- the in and uncertainty incompleteness tistical for corrects self-consistently that (BLQSOs) quasars line Abstract: Keywords: Eprint: Aneta Siemiginowska, Lars; Hernquist, Authors: Function Mass Hole Black Quasar Broad Line Lifetimes, SDSS the Quasar from Distributions Growth, Ratio Eddington and Hole Black on Constraints Eprint: Authors: accreting the unbinds feedback hole flow. black accretion when the event halting fueling gas, a of end the at occurs http://arxiv.org/abs/1006.3561 http://arxiv.org/abs/1006.3788 hrbr,Jonathan Thornburg, el,BadnC;Vsegad aine a,Xahi okn,Philip; Hopkins, Xiaohui; Fan, Marianne; Vestergaard, C.; Brandon Kelly, esuytesottr fet fa nemdaems lc oe(IBH) hole black mass intermediate an of effects short-term the study We epeeta siaeo h lc oems ucin(HF fbroad of (BHMF) function mass hole black the of estimate an present We sr-hC;atohsc;osrain;sprasv lc holes black supermassive observations; astrophysics; astro-ph.CO; udmna hsc ihLISA with physics Fundamental M BH < 10 WNotes GW 9 M

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49 oe esfrG science GW for News & Notes Notes & News for GW science 50 WNotes GW oeo mass of mass hole of "particle" small a If Abstract: Keywords: oegaiainlwv mltd,gvni em ftno peia harmonics. spherical tensor of terms far- in the given to amplitude, corrections particle wave mass point gravitational (1pN) arbitrary zone post-Newtonian of first binaries the compact including nonspinning ratio eccentric for forms wave itational Abstract: forms Keywords: Eprint: Authors: binaries compact eccentric from forms gravita- wave tional 1pN-accurate frequency-domain Full-analytic regularized of sum infinite an as self-force the modes gives spherical-harmonic formalism a of mode-sum problem The spacetime. model Schwarzschild the in orbit on geodesic focus circular I allows a in yet orbits. particle efficient, scalar particle is arbitrary this to adaptive-mesh- formalism; generalization regularization an easy mode-sum use Barack-Ori I the equations perturbation in computation. the of the integration numerical for time-domain (AMR) estimates refinement error validating error (relative and accurately ing highly self-force this compute to of valuable it’s that argue I ei,Ioti h cnrvrat ailcmoeto h effrefrapril in particle radius a areal for of self-force orbit the arith- geodesic of circular floating-point component a radial extended-precision (contravariant) the and obtain refinement, I metic, mesh fixed AMR, similar have Using to functions basis but the ill-conditioned, renormalizing numerically by is alleviated magnitudes. fit mostly tail be the can that show this I self-force. the computing in errors numerical actual ` the that accuracies. widely-varying evidence of numerical computations present self-force I numerical of set large a using oi ti"sre.Hr aiaeteitra ro siae o h individual the for estimates error internal the validate I Here series. "tail" totic for numerically computed r tms ekycreae,s h sa ttsia ro siae r ai for valid are estimates error statistical usual the so correlated, weakly most at are . 10 − http://arxiv.org/abs/1006.3714 6 n fcety n ecietcnqe o on hsadfrobtain- for and this doing for techniques describe I and efficiently, and ) ese,Mne;Shee,Gerhard Schaefer, Manuel; Tessmer, h ril rvdsrayt-s p-cuaefeunydmi grav- frequency-domain 1pN-accurate ready-to-use provides article The MI rq;sl force self gr-qc; EMRI; rq;msiebnre fbakhls otNwointer;wave- theory; post-Newtonian holes; black of binaries massive gr-qc; M h atcei ujc oan to subject is particle the , udmna hsc ihLISA with physics Fundamental ` P µ . ` ∞ M = 0 30 F (with `, n siae o larger for estimated and reg with , µ r  = Ø( 10 1 F risaShazcido erblack Kerr or Schwarzschild a orbits ) µ `, M reg ) aito-ecin"effre.Here "self-force". radiation-reaction owithin to etme ,2010 7, September ada itra"errestimate) error "internal" an (and 1 ∼ ∼ ` p eaieerror. relative ppm yfitn nasymp- an fitting by F `, reg o different for F

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reg ∼ oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 unydet aito ecinaeue opoiesainr hs approxima- phase fre- stationary forms. radial provide wave of to frequency-domain growth the used and to are tions eccentricity reaction the radiation to of due decay quency the for equations averaged The ae yRdaieFebc .ShrclSmercAc- Symmetric Regu- Spherical cretion I. Holes Feedback Black Radiative by Mass lated Intermediate onto Accretion field speed large the at Alfven to suppressed toroidal relative is corresponding width instability the the fractional unity), with the than strengths (with less tori much thin radius mag- For significant torus various have outer instability: with fields PP magnetic tori effect the toroidal incompressible on the general, effects in study In We instability structures. and PP magnetized. strengths the highly netic on be fields to However, magnetic likely are of rate. mergers) neu- rotation and binary collapsars fluid star (e.g., situations tron the astrophysical matches various in speed produced tori pattern accretion corotation wave the the across where waves non-axisymmetric radius, of insta- interaction (PP) the Papaloizou-Pringle from so-called arising bility, the instability, hydrodynamical global a to Abstract: holes Keywords: Eprint: Authors: Tori Accretion Magnetized of Instability Papaloizou-Pringle Keywords: Eprint: Authors: or sufficiently 0.4 for order in of sets width (with instability fractional fields the the magnetic stable, (with strong hydrodynamically tori are thicker which For larger), rate). rotation flow the asbakholes black mass stable is it when even instability instability. global magneto-rotational to usual subjected the against be may tori accretion netized http://arxiv.org/abs/1006.3824 http://arxiv.org/abs/1006.1302 u e;Li Dong Lai, Wen; Fu, ak wnH;Rcti Massimo Ricotti, KwangHo; Park, o crto oiaon opc betaekont esusceptible be to known are object compact a around tori accretion Hot crto ic;atop.E Mcutrat;msiebnre fblack of binaries massive counterparts; EM astro-ph.HE; discs; accretion crto ic;atop.O sr-hH;atohsc;intermediate- astrophysics; astro-ph.HE; astro-ph.CO; discs; accretion udmna hsc ihLISA with physics Fundamental v A φ & 0 . 2 WNotes GW r Ω .Orrslssgetta ihymag- highly that suggest results Our ). v A φ & 0 . 2 r Ω (where Ω is

51 oe esfrG science GW for News & Notes Notes & News for GW science 52 WNotes GW fse lc oe nteeryuies n omk rdcino h number the of prediction IMBHs a by medium. produced make interstellar galaxies the to in from sources and growth accreting X-ray the universe ultra-luminous model early of to luminosity the step the in and first radi- holes a of is black spectrum study seed softer This that of find rate. also accretion proportional We higher is sphere. produces bursts Strömgren ation the the of of cru- period size is the mean the while gas to rate, ionized feedback accretion hot the how the determining of of in formulation profile cial a temperature provide The thus operates. and accretion bursts and regulated the rate accretion of mean luminosity the peak bursts, between the period the for formulas parametric rive 3-6% siltr eairo h crto ae ihdt cycle duty with rate, accretion the of behavior oscillatory tempera- and density masses, ture, hole different black including spectra, space, radiation and of parameter efficiencies suite large radiative a a present We across properties. accretion flow mean exploring the simulations affect rate de- not accretion that do hydro-instabilities simulations similar the 2D show that in meaning velop simulations gas accretion, 2D the in peaks and regulates between 1D hole period Both black and the simulations scales. near 2D large emitted and from radiation 1D supply UV Our from and momentum. accretion X-ray assume angular how we zero explore series, with a gas of dense first radia- uniformly the a paper, a with this ZEUS-MP In code algorithm. hydrodynamical transfer the tive using (IMBHs) holes black mass Abstract: ttoa noneswt e oa fet epeettommn oesthat models moment two present We effect. grav- two-body local of statistical net number In large a a with system. of result a encounters the such itational is of relaxation that of evolution are assume number global we they a models the are neighborhood; model There solar to relaxation. densities the techniques to high related different in processes very than study the higher to to laboratories times due unique dynamics million stellar a study usually to reached, loci ideal are clusters star Abstract: dynamics Keywords: Eprint: Authors: dis- velocity stellar function the tribution of systems: modeling stellar the dense to of Applications models moment order Higher T ( T ∞ ∞ http://arxiv.org/abs/1006.1365 ftenihoiggs nareetwt rvossuisw n regular find we studies previous with agreement In gas. neighboring the of , / cnie,Jsu;AaoSon,Pu pre,Rainer Spurzem, Pau; Amaro-Seoane, Justus; Schneider, es tla ytm uha lblrcutr,glci uliadnuclear and nuclei galactic clusters, globular as such systems stellar Dense esuyteefc frdaiefebc naceinot intermediate onto accretion on feedback radiative of effect the study We 10 sr-hC;atop.A srpyis lblrcutr;g-c stellar gr-qc; clusters; globular astrophysics; astro-ph.GA; astro-ph.CO; 4 K) 2 . 5 fteBnirt n ekaccretion peak and rate Bondi the of udmna hsc ihLISA with physics Fundamental etme ,2010 7, September ∼ 10 ∼ 7%

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enaceinrate accretion mean , oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 losu odrv eoiydsrbto ucin ihupeeetdaccuracy, unprecedented with models. function, moment distribution model previous resulting velocity to The compared a stars. derive velocity de- to high more of us in number allows mechanisms the decrease study Since or can increase series. we that infinite moments tail the order from fourth included include by moments models model of both number our the of on anisotropy relies approach of equations order degree moment of the of moments set constrain expressing the which computed complete relations We are closure and potentials. relaxation with Rosenbluth two-body the for of account means equations by moment the of side order at and where equations moment order differential Boltz- of of the moment the of set for moments infinite equation the taking an By obtains one equation. equation Boltzmann mann collisional the on based are eigo ra-ieeiso rgntn rmteatv opnn fa SMBH an of scat- component of wind. active terms outflowing the an in from from explained or originating binary, be emission and can broad-line hypothesis observations recoil of our the tering of whether implications consider the some briefly to discuss We velocity bound also a galaxy. gas with host as moving the identified itself to is is ative system SMBH the velocity that high at implies the region this If SMBH, scattering galaxy. a host towards the and in observer with rest the moving from components, away two velocities has bulk region a different broad-line with the consistent which are in observations these model that scattering show We asymmetry. by blue strong redshifted a are and broad lines the Balmer flux polarized broad in whereas the flux, to total due In ∼ recoil binary. gravitational supermassive (SMBH) a of of hole example merger the black an following waves be gravitational may of emission it anisotropic that suggest which (z=0.297), Abstract: observations Keywords: Eprint: E. James Authors: E1821+643 Quasar the in hole black supermassive kicked a for evidence Spectropolarimetric etuct h nnt e fmmn qain torder equilibrium. at dynamical equations require moment of not set do infinite we the but truncate symmetry We spherical assume we els 00k/ eaiet h arwlnsadhv ihyrdaymti profiles, asymmetric red highly have and lines narrow the to relative km/s 1000 http://arxiv.org/abs/1006.0993 oisn nrw on,Sur;Ao,DvdJ;Kab rei Smith, Preeti; Kharb, J.; David Axon, Stuart; Young, Andrew; Robinson, erpr pcrplrmti bevtoso h usrE1821+643 quasar the of observations spectropolarimetric report We sr-hC;atohsc;kcsrci;msiebnre fbakholes; black of binaries massive kicks/recoil; astrophysics; astro-ph.CO; n = 5 o h eodmdl h olsoa em nteright-hand the on terms collisional The model. second the for udmna hsc ihLISA with physics Fundamental n + 1 H ymmnso order of moments by n α otismmnso order of moments contains ieehbt lehf fsmlrmagnitude similar of blueshift a exhibits line WNotes GW n n h cuayo this of accuracy The . = 4 o h rtmodel first the for n ∼ + 10k/ rel- km/s 2100 1 normod- our In .

53 oe esfrG science GW for News & Notes Notes & News for GW science 54 WNotes GW grsmyhv infiatipc ntesga oeln,o oredetection, algorithms. source estimation on parameter modelling, of signal development the the on on and impact significant a have may figures tnadMH ouainmdl,orrslspeitecnrcte nteranges the in to eccentricities applied predict When results 10 our binaries. models, mass population unequal MBHB general, standard for and/or in especially eccentric eccentricity, that, MBHB mildly find the already We of initially increase refilling. dramatic cone a loss causes distribution, dynamics of density stellar binary efficiency stellar the the the and of are slope normalization which the its eccentricity, system initial the and tracks ratio of evolutionary mass parameters mass, of relevant family a the produce sampling We extensively campaigns. (PTA) array the timing with pulsar ( detection its Antenna GW addressing for Space of impact Interferometer possible Laser attempt its planned the and in process eccentricity, merger binary the main the in Our of importance refilling. behaviour cone the loss on binary stellar is the the of focus of efficiency evolution the the for of for and framework experiments distribution analytical density scattering an 3-body to hy- stars numerical a unbound of in and results treated bound cone, the is loss dynamics coupling binary Stellar by the fashion (GWs). brid waves feeding gravitational stars the of unbound to emission bound of the cusp and scattering stellar central the the binary holes, of the black erosion of the massive dynamics account into The taking stars. by of evolved distribution is surrounding a in embedded HBs) Abstract: dynamics Keywords: Eprint: Authors: observations impli- wave environments: gravitational for stellar cations in binaries hole mas- eccentric black of sive evolution the for model consistent Self Eprint: Star Authors: of simulations for code Clusters N-body new A MYRIAD: − 3 − 0 http://arxiv.org/abs/1006.3326 http://arxiv.org/abs/1006.0730 . 2 eaa A. Sesana, osatnds io;Kkoa,Ksa D. Kostas Kokkotas, Simos; Konstantinidis, and ecntuteouinr rcsfrmsiebakhl iais(MB- binaries hole black massive for tracks evolutionary construct We sr-hC;atohsc;g-c asv iaiso lc oe;stellar holes; black of binaries massive gr-qc; astrophysics; astro-ph.CO; 0 . 03 − 0 . 3 o ore eetbeby detectable sources for udmna hsc ihLISA with physics Fundamental LISA etme ,2010 7, September LISA ,adogigadforthcoming and ongoing and ),

n T epciey Such respectively. PTA and oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 fPumrmdl ossigo qa-assasrahdcr olpea t at collapse core reached Simulations stars collapse. equal-mass core of beyond consisting and to and models up accuracy Plummer good clusters of a star give of by parameters simulations replaced free for the be speed of could Processing choice GRAPE-6, Graphics Appropriate uses the (GPUs). that like Units accelerating-hardware code other the uses of that eas- module part be another the can it that Moreover, so appro- binaries. modified black-hole the evolution, ily close binary allows of and evolution and stellar and as modular collisions such is stellar the phenomena, code physical in more the exist of of or treatment encoun- priate structure dynamically close form The for either configuration. used that initial sub-systems is are multiple treatment particles and steps, Special neighboring binary and time board. ters, forces block GRAPE-6 the with the while scheme using time, fourth-order computed in particles Hermite the the advancing uses for code The clusters. Abstract: super- dynamics; stellar methods; holes numerical black massive holes; black intermediate-mass hw; Keywords: Eprint: Gustavo beroff, Authors: dy- inspiral hole namics black binary on constraints Statistical close for used is that method the of accuracy high sub-systems. in the multiple created to and dynamically due binary is is systems accuracy This binary close the simulation. of than a number better a even when codes, and existing comparable of becomes accuracy code collapse the core Finally, reached literature, an the with in t models found at those King to of different similar Simulations for mass-function, collapse compar- initial agreement. core Also, of excellent time show the 0.001. for conditions, below codes initial other remained of energy results while published the results, with in existing isons error with relative well cumulative very compares the which times, relaxation half-mass ee pc fiiilcngrtosfrqaicrua nprl.Truhaprincipal a Through inspirals. quasi-circular for configurations para- initial the of evolving space and meter sampling systematically by approximation post-Newtonian Abstract: holes black supermassive spin; theory; post-Newtonian relativity; numerical holes; Keywords: ∼ .7 hc ssihl mle hnteepce eutfo rvosworks. previous from result expected the than smaller slightly is which 0.17, http://arxiv.org/abs/1005.5560 aly hdR;Hrmn,Fak ibroz on ilo aul Guer- Manuel; Tiglio, John; Silberholz, Frank; Herrmann, R.; Chad Galley, epromasaitclaayi ftebnr lc oepolmi the in problem hole black binary the of analysis statistical a perform We epeetanwC+cd o olsoa -oysmltoso star of simulations N-body collisional for code C++ new a present We sr-hG;atop.M srpyis lblrcutr;GU GRAPE GPU; clusters; globular astrophysics; astro-ph.IM; astro-ph.GA; P;g-c nemdaems lc oe;msiebnre fblack of binaries massive holes; black intermediate-mass gr-qc; GPU; udmna hsc ihLISA with physics Fundamental WNotes GW ∼ 17

55 oe esfrG science GW for News & Notes Notes & News for GW science 56 WNotes GW fgaiainlwvsfrgaiainlwv detectors. wave gravitational templates for of these building waves applications numerical gravitational other and of semi-analytical Among in regimes. both useful merger be and should to inspiral results over of the carry simulations in might results theory hole these full black extent for the what binary account to present that analyzing We equations variables Einstein the problem. full the find the and in variations for to variations look respect largest also with the We and time orientations. of con- spin functions highly initial as are in both which sense, them statistical of a three in find served systemat- and we quantities uncorrelated variables for momentum look angular ically orbital and spin of analysis component n hsclocrigi ayohrglci uli h etro u Milky our of Center The nuclei. galactic other many in occurring physical and Abstract: holes black Keywords: Eprint: Authors: Way the Milky in the Cluster of Star Center Nuclear and Hole Black Massive The to re- counterparts these electromagnetic of producing applications for astrophysical mechanism signals. of a gravitational-wave as number particular a in discuss sults, We stability. in the gains while case, stable, Newtonian less purely slightly system comes the the binary to that Relative the find as losses. we problem radiation three-body gravitational restricted via circular evolves the in points librium Abstract: holes black Keywords: Eprint: Authors: System Binary Hole Points Equilibrium Lagrange The http://arxiv.org/abs/1006.0064 http://arxiv.org/abs/1006.0182 ezl enad iehur rn;Glesn Stefan Gillessen, Frank; Eisenhauer, Reinhard; Genzel, D. Jeremy Schnittman, h aatcCne sa xeln aoaoyfrsuyn phenomena studying for laboratory excellent an is Center Galactic The ecluaetelcto n tblt fthe of stability and location the calculate We sr-hH;atohsc;E oneprs rq;msiebnre of binaries massive gr-qc; counterparts; EM astrophysics; astro-ph.HE; sr-hG;atohsc;osrain;SgtaisA;supermassive A*; Sagittarius observations; astrophysics; astro-ph.GA; L 4 qiiru on oe oad h eodr asadbe- and mass secondary the towards moves point equilibrium udmna hsc ihLISA with physics Fundamental L 5 on oe wyfo h eodr and secondary the from away moves point etme ,2010 7, September L 4 and L 4 and L

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naBlack a in arneequi- Lagrange oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 einn odlnaetepyia rprisi h o crto oeaon the is around emission zone this accretion how hot and the in A* horizon. properties event Sgr physical onto the gas delineate accreting to about beginning the known is of what properties briefly un- more emission ’stellar fully summarize the not equilibrium also presently We an and youth’. remarkable young of of a ’paradox of constitutes properties derstood mainly This predicted consist hole. black the to a appears to around cusp’ cluster’ contrast ’S-star in peri-bothroi This stars, orbital day. have early-type light which one of im- than three the hole, less in black of centered massive stars stellar the fainter top-heavy of of a vicinity concentration with mediate dense have apparently a recently, stars discuss A* We that Sgr star function. fact of nuclear mass astounding vicinity dense the the the in including of forming hole, been evolution black and this structure surrounding the about cluster known is what report eamsiebakhl fabout must source of radio hole this that black A*, size massive Sgr the source, a of radio measurements be compact the from central and the stars of dozen motion two and than analy- more the of from orbits of evidence, the properties current of the the sis present on the We and cluster. on hole star emphasis dense black strong surrounding massive the a central with a for parsec, evidence central empirical the current on obser- work in theoretical progress and recent ex- electromagnetic the vational in summarizes of review powerful reso- This energy more measurements. exquisite increasingly in these become with plaining magnitude have observations of simulations orders and Theoretical 18 nucleus, radiation. cover galactic sensitivity closest and the lution far by is Way xiisasrn ap h oml otema ria lnsi h ne n outer and by inner differ the in disc planes or orbital the one, mean of the occupy to third normals stars the the warp: strong that a radii showing exhibits of as discs interpreted two, be can possibly centre Galactic the in Abstract: Keywords: Eprint: in Authors: disc stellar the centre of Galactic warp the the and relaxation Resonant etrrsnn eaainbtenteds n h urudn l tla cluster. stellar old through surrounding the inevitably and and disc naturally the arise between relaxation warps resonant such vector that show we theory, Lagrange http://arxiv.org/abs/1006.0001 oss ec;Tean,Scott Tremaine, Bence; Kocsis, bevtoso h pta itiuinadknmtc fyugstars young of kinematics and distribution spatial the of Observations sr-hG;atohsc;SgtaisA;selrdynamics stellar A*; Sagittarius astrophysics; astro-ph.GA; udmna hsc ihLISA with physics Fundamental ∼ ∼ 0dg sn naayia oe ae nLaplace- on based model analytical an Using deg. 60 .505p.Tems rmnn ‘lcws’ disc (‘clockwise’) prominent most The pc. 0.05-0.5 4 . 4 x 10 WNotes GW 6 M

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57 oe esfrG science GW for News & Notes Notes & News for GW science 58 WNotes GW h pncnrbtost h nryflxadpaeeouint NLO. compute to to evolution paper phase separate and a flux energy in the used to be contributions dy- will spin spin that the necessary formalism the EFT of canonical the a calculation within using the Newton- dynamics namics completes correct al. the then the paper of et to This leads application Faye algebra. action direct the (Dirac) by of the level results the that at previous show SSC Wigner with also We equivalence the condition arXiv:gr-qc/0605139. supplementarity in prove in- spin explicitly of covariant potential and the use gravitational (SSC), We the binaries. to compact contributions spiralling spin-orbit (NLO) order leading Abstract: Keywords: Eprint: Authors: of motion the binaries in compact effects inspiralling spin-orbit order leading to Next Eprint: Authors: gravity in Chern-Simons holes dynamical black Schwarzschild of signature Gravitational sources. of other in r-modes available the readily not with is connection that stars) (in treatment neutron a radiation of contain remain gravitational they lectures because current-quadrupole The particular and of in sources, waves. and gravitational reasons, their pedagogical detecting waves, for for interest gravitational time linearized the at of prospects theory the the covering 1999, in Abstract: Keywords: Eprint: Authors: Detectors and Sources, Waves, Gravitational http://arxiv.org/abs/1004.4007 http://arxiv.org/abs/1005.4735 http://arxiv.org/abs/1005.5730 ot,Rfe A. Rafael Porto, oia . ai al;Croo io;Gatei Leonardo Gualtieri, Vitor; Cardoso, Paolo; Pani, C.; Molina, Franco Ricci, F; Bernard Schutz, oe flcue o rdaesuet htwr ie tLk Como Lake at given were that students graduate for lectures of Notes sn fetv edter ET ehiusw aclt h next-to- the calculate we techniques (EFT) theory field effective Using sr-hC;g-c e-h e-h asv iaiso lc oe;spin holes; black of binaries massive hep-th; hep-ph; gr-qc; astro-ph.CO; sr-hH;g-c oe flectures of notes gr-qc; astro-ph.HE; udmna hsc ihLISA with physics Fundamental

etme ,2010 7, September oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 litct fteodrof order the of ellipticity meth- domain frequency and numerically. evolution appearance time their both verify ods. using explicitly validated we are and results constant, arise, Our coupling the to gravitational- of known values with This negative are tested For field. be ghosts LISA. or scalar could LIGO and the as theory such to detectors, Chern-Simons coupling wave for the gun of smoking imprints a oscil- carry gravitational is holes the black Thus, of field. scalar modes grav- die the lation the by Relativity, perturbations driven General also small standard are to and waveforms contrast itational in stable, However, are ringdown. vanishes. spacetimes a as field these away scalar that background suggest the results that Our assuming sym- parity-violating spherically spacetimes, a of hole perturbations through black study field metric we scalar framework, a this In to term. coupled Chern-Simons is field gravitational the which Abstract: theories Keywords: eddt banngtv uduoeelpiiis hl ed ofie otecrust the ellipticities. to quadrupole confined positive fields produce normally while typically is ellipticities, star quadrupole whole to negative the obtain comparable permeating to is field needed fields magnetic A magnetic quadrupolar components. dipolar of of effect that The to up with case). ellipticities extreme stars (quadrupole most deformations neutron the larger for to subject that, principle in show are results Our of star. equation the the the 1.4 explore of = of also M mass We choice mass the particular shape. the on prolate on and a deformation has state stellar star the the of which for dependence those spe- to paying attention configurations, field cial different and by included. poloidal induced also deformations both are the multipoles having evaluate order We fields higher magnetic and study, considered, perturbation our are a components In as toroidal star. acts neutron field magnetic spherical the a which of in approach, linear a with equations Abstract: Keywords: Eprint: Authors: defor- and structure mations magnetars: of models Relativistic http://arxiv.org/abs/0712.2162 oaua . err,V;Gatei . os .A. J. Pons, L.; Gualtieri, V.; Ferrari, A.; Colaiuda, efidnmrclsltoso h ope ytmo Einstein-Maxwell’s of system coupled the of solutions numerical find We yaia hr-iosgaiyi netnino eea eaiiyin Relativity General of extension an is gravity Chern-Simons Dynamical sr-hH;g-c e-h e-h ierzdter;tsso alternative of tests theory; linearized hep-th; hep-ph; gr-qc; astro-ph.HE; sr-h sr-hS;gnrlrltvt;gr-qc relativity; general astro-ph.SR; astro-ph; M

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59 oe esfrG science GW for News & Notes Notes & News for GW science 60 WNotes GW aatcsucsaddsusterdtcaiiywt urn n uuegravitational future extra- and by current observatories. with produced wave detectability backgrounds their discuss for and predictions contribution, sources this theoretical galactic In recent detection. review future is possible, will it a we that of features view and in properties investigate spectral to different astrophysi- important has specific component a of Each to result associated process. the each cal is components, which different background waves of a These superposition form the and formation. Universe, galaxy redshift and high star our of permeate beginning the since occurred processes Abstract: Keywords: Eprint: Authors: ex- sources from tragalactic waves gravitational of backgrounds Stochastic ubro ao oacutfrtez6qaa BHs. quasar sufficient z=6 a the contain for regions account these to halos B-field; of fluctuating (2-3)- number rare spatially the the in of realized regions be can sigma it However, (CMB). background sup- microwave permanently cosmic to required strength field press magnetic critical The near stays densities. higher temperature gas the and (T= cient, warm kept is gas has of collapsing field density the the critical nG, the If reaches (comoving) it diffusion. 3.6 until mag- ambipolar = primordial via B strong above gas sufficiently strength collapsing a a the of heats presence which T= the field, near in netic temperatures satisfied at be remain can to condition gas the and requires cooling This (SMBH). avoid hole black to supermassive a in resulting possibly lapse, above temperatures virial Abstract: Keywords: Eprint: Authors: Field Magnetic Redshifts Primordial High a at Through Formation Hole Black Supermassive H 2 H prahlcltemdnmcequilibrium. thermodynamic local approach http://arxiv.org/abs/1005.2942 http://arxiv.org/abs/1005.0977 2 coigi oehthge hnuprlmto prx Gfo the from nG 2 approx. of limit upper than higher somewhat is -cooling cnie,Rfala aas,Seai;Frai Valeria Ferrari, Stefania; Marassi, Raffaella; Schneider, eh,Si . amn otn ady Kanhaiya Pandey, Zoltán; Haiman, K.; Shiv Sethi, thsbe rpsdta rmrilgsi al akmte ao,with halos, matter dark early in gas primordial that proposed been has It srpyia ore mtgaiainlwvsi ag ait of variety large a in waves gravitational emit sources Astrophysical sr-hC;bc/oerud omlg;gr-qc cosmology; back/foreground; astro-ph.CO; sr-hC;csooy uemsiebakholes black supermassive cosmology; astro-ph.CO; udmna hsc ihLISA with physics Fundamental 10 4 ,cnaodfamnainadudrorpdcol- rapid undergo and fragmentation avoid can K, n crit = 10 3 10 cm 4 ,ee si otne oclas to collapse to continues it as even K, − 3 etme ,2010 7, September twihtert-irtoa states roto-vibrational the which at H 2 coigte ean ineffi- remains then -cooling 10 4 .W hwta this that show We K. 10

4 K) oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 ie feto pnobtpeeso n rvttoa aito ed oaspin-flip a to leads radiation gravitational com- and the precession cases, (1/30,1/3) spin-orbit possible range of all even ratio of effect logarithmically mass 40% bined representing the a mergers In hole establish encounter. black to their supermassive at of then ratios distribution, mass the mass of their probability derive enables unexpected to which to candidates, first hole lead black us can supermassive which of statistics parameter, a small present We second results. a provides one from ferent Abstract: theory Keywords: Eprint: Authors: inspiral the during spin-flip hole black Supermassive compo- perturbing the of property morphological and nents. some measurements evaluate the these with to of compared used expansion be possibly the can that in solutions contributions secular linear produces matter simple fields dark sta- of local global a inclusion a or The dust and interplanetary precession component. the slow like a sources to for associated responsible by field, field given tionary those Solar previ- are the in perturbations to assumed autonomous corrections that of the than classes longer relevant is Other mission global the papers. the of injection ous base-line on as- of time implications interpretation Earth the possible accurate the when on orbit of light An in sheds field solution frame. tidal perturbed Hill the the the of on structure in put stationary is be emphasis orbits. to particular Keplerian sumed a purely to work perturbations present the the analyze has In to orbits is orbits. forward LISA unperturbed step the optimal natural find of a to The on study frame based the Hill techniques the in position, analytical in step implement the approximation first which "post-epicyclic" of papers This recent terms of frame. in subject Hill only the the been expressed in be time can of not that but fields by produced effects the Abstract: Keywords: Eprint: Authors: orbits LISA of perturbations Autonomous http://arxiv.org/abs/1005.2976 http://arxiv.org/abs/1005.2287 egl,Lsl . iran ee . aaee arni I. Laurentiu Caramete, L.; Peter Biermann, A.; Laszlo Gergely, Massimo Visco, Massimo; Bassan, Giuseppe; Pucacco, eivsiaeatnmu etrain nteobt fLS,namely LISA, of orbits the on perturbations autonomous investigate We uigps-etna vlto facmatbnr,ams ai dif- ratio mass a binary, compact a of evolution post-Newtonian During eetr;g-c ntuet;interferometers instruments; gr-qc; detectors; sr-hC;g-c asv iaiso lc oe;post-Newtonian holes; black of binaries massive gr-qc; astro-ph.CO; udmna hsc ihLISA with physics Fundamental WNotes GW

61 oe esfrG science GW for News & Notes Notes & News for GW science 62 WNotes GW nua oetm eas eieafruafrtefia pna h n fthe of end the at spin final orbital the and range. for spin ratio formula mass the this a of as in derive orientation inspiral inspiral also relative We the original during and momentum. occurring ratio angular angle mass spin-flip the plunge. the the of during of function the occur magnitude in may it while the (1/3,1) happens, analyze ratios We never mass an- with spin-flip In mergers a of galaxies. (1/30,1/1000) 20% radio ratios remaining X-shaped mass on with observations mech- of 40%, a set provides other large This merger. a the explaining of for phase inspiral anism the during spin dominant the of l f37+-1 ere n scnitn ihtejtai.Ti ugssteactive the suggests This axis. jet the with consistent is an- and position degrees a hole, 17 along black is +/- displacement 307 supermassive The of the galaxy. gle the of of location photo-center ( the the and be pc SMBH) to 0.8 (presumed +/- source 6.8 point of nuclear displacement projected a reveals veys, Abstract: holes black supermassive observations; holes; black of naries Keywords: Eprint: Authors: M87 in Hole Black Supermassive Displaced A scheme. measurement LISA the post-processing in of noise validation phase experimental clock first and the noise marks frequency laser of removal This bed. LISA. in approximately occur by by will noise lab- that frequency a couplings laser in noise suppressed implemented the TDI was mimic TDI to designed Antenna. experiment Space oratory Interferometer Laser the LISA, for Abstract: det Keywords: Eprint: A. Daniel Shaddock, M.; William Authors: Antenna Space Interferometer Laser the for etry Interferom- Time-Delay of Demonstration Experimental 6 × 10 http://arxiv.org/abs/1005.2173 http://arxiv.org/abs/1005.2176 4 acedr . oisn . xn .J;Prmn .S;Mrit D. Merritt, S.; E. Perlman, J.; D. Axon, A.; Robinson, D.; Batcheldor, eVn,Gen ae rn;MKni,Kr;Seo oetE;Klipstein, E.; Robert Spero, Kirk; McKenzie, Brent; Ware, Glenn; Vine, de spoa nlsso 8,uigdt rmteAvne aeafrSur- for Camera Advanced the from data using M87, of analysis Isophotal erpr ntefis eosrto ftm-ea nefrmty(TDI) interferometry time-delay of demonstration first the on report We eoeigteitiscdslcmn os oro u aoaoytest laboratory our of floor noise displacement intrinsic the recovering , sr-hC;atohsc;gaiainlrci;kcsrci;msiebi- massive kicks/recoil; recoil; gravitational astrophysics; astro-ph.CO; sr-hI;dtcos rq;isrmns nefrmtr;physics.ins- interferometers; instruments; gr-qc; detectors; astro-ph.IM; udmna hsc ihLISA with physics Fundamental etme ,2010 7, September 10 ∼

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. rsc ewe the between arcsec) 0.1 n lc hs noise phase clock and oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 ag eolta curdi h femt famjrmre n iei h last the in time any merger major a of offset. aftermath observed the Gyr. the in 10 from produce occurred resulting that can oscillations recoil and residual large to axis, a due jet be the could displacement with the aligned Alternatively, be could disk, gas etrn oc sngiil.Ti ol etecs ntelwdniycr fM87. of core density low the galaxy in the case if and the recoil Gyr be 0.1 moderate could > A This of age negligible. jet is a is for force asymmetry rate, restoring jet accretion However, observed the mechanisms. at dis- viable, two The only latter binary. SMBH the an favors of direction coalescence placement the jet, from one-sided resulting intrinsically recoil or gravitational asymmetric objects and an massive by to acceleration due clusters), or- perturbations globular include gravitational (e.g., binary, displacement SMBH the an for of displaced explanations motion is but bital Possible mass, of direction. center counter-jet galaxy the the at in reside currently not does M87 in SMBH olsigbnre t2N fteodrof order for the eccentricity of residual ec- a zero 2PN, induce the at couplings in binaries spin-spin divergencies coalescing that of find We free use orbit We limit. order. the centricity (PN) of post-Newtonian parametrization second quasi-Keplerian the at a orbits comparable- eccentric by on emitted binaries waves mass gravitational of phasing the of computation accurate Abstract: waveforms theory; Keywords: Eprint: Authors: from waves orbits gravitational eccentric on of binaries phasing the in effects Spin Eprint: Array Authors: Timing Pulsar a in Bursts Wave tional Gravita- of Characterization and Localization Detection, the on errors the measurement. reduce wave gravitational to a help in spins could and pattern which eccentricity non-trivial eccentricity, the of a the determination induces of also evolution precession the Spin-orbit in band. LISA the in binaries http://arxiv.org/abs/1005.2046 http://arxiv.org/abs/1004.3499 li,Atie ezr Philippe Jetzer, Antoine; Klein, in e aul omn nraN. Andrea Lommen, Samuel; Lee Finn, ecmuehr h pnobtadsi-pnculnsnee o an for needed couplings spin-spin and spin-orbit the here compute We sr-hC;g-c asv iaiso lc oe;post-Newtonian holes; black of binaries massive gr-qc; astro-ph.CO; ∼ y g ih xli h itre aueo h nuclear the of nature disturbed the explain might ago Myr 1 udmna hsc ihLISA with physics Fundamental WNotes GW 10 − 4 - 10 − 3 o uemsiebakhole black supermassive for

63 oe esfrG science GW for News & Notes Notes & News for GW science 64 WNotes GW hs uss u nlssadess namtal ossetmne,ahierar- a manner, consistent characterize mutually and a detect in to questions: addresses, three analyzed de- of analysis be chy we Our Here may data strings. bursts. cosmic array highly these on timing cusps in pulsar or objects super- SMBH, how compact of a scribe of coalescence about passage orbits or unbound periapsis formation or the the elliptic (SMBHs), include Sources holes bursts waveband. black detectable array massive timing to pulsar rise the the give in than arise shorter that also much will is — duration whose period signals observation — bursts sig- wave periodic or Gravitational stochastic nals. e.g., waves: gravitational stationary on traditionally cused Abstract: wave- holes; forms black supermassive resolution; sky algorithms; search physics.data-an; Keywords: ueSBB,te h fego ol eitrrtda intr ftebirth the of signature pro- a that as mergers interpreted galaxy be major could same afterglow the the by then triggered SMBHBs, the is duce of activity hardness spectral quasar by the If characterized in and is source. luminosity window, bolometric sensitivity the LISA’s both lasts in in increases which SMBHBs afterglow, rapid for viscous decades The and to alone. bright years surveys sufficiently for EM be in may detectable afterglows be the to whether numerous the study of we counterpart EM Here the pro- source. identify help been LISA LISA, can by has afterglow (GWs) this It waves for gravitational searches merger. in EM detected follow-up the been has after merger disk the once gas viscous that posed the circumbinary by surrounding produced the afterglow, of (EM) electromagnetic infall an by accompanied be to Abstract: holes Keywords: Eprint: Authors: Quasar a of Birth the Witnessing data. to detector applicable space-based directly or is ground itself either using analysis detection the wave gravitational arrays, gravitational is timing discussion pulsar our via of context detection the wave While determined. be and to waveform, waveform the the infer of source the localize and either tect to can weak we too that is find radiation the we analy- sets our data Applying synthetic states? to polarization its sis of each in dependence time waveform’s and source? its to burst? wave gravitational http://arxiv.org/abs/1004.5411 oaiesucsee hnterdainapiuei o ekt permit to weak too is amplitude radiation the when even sources localize aaa aais;Hia,Zla;Mnu Kristen Menou, Zoltan; Haiman, Takamitsu; Tanaka, fot odtc rvttoa ae ytmn naryo usr aefo- have pulsars of array an timing by waves gravitational detect to Efforts h olsec fasprasv lc oebnr SBB sthought is (SMBHB) binary hole black supermassive a of coalescence The sr-hC;atohsc;E oneprs asv iaiso black of binaries massive counterparts; EM astrophysics; astro-ph.CO; sr-hI;brt;dt nlss rq;prmtrestimation; parameter gr-qc; analysis; data bursts; astro-ph.IM; i)Asmn h us rpgto ieto,wa steburst the is what direction, propagation burst the Assuming iii) )Wa r h dsta aae nldstesga rma from signal the includes dataset a that odds the are What i) udmna hsc ihLISA with physics Fundamental i suigtepeec fabrt hti h direction the is what burst, a of presence the Assuming ii) eetgaiainlwvsee when even waves gravitational detect etme ,2010 7, September

de- oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 egn.Ti enocstento htjitE-lsG bevtosofrthe mergers. offer SMBHB observations of signatures EM-plus-GW EM joint the that identifying chal- for notion remain prospects likely the best be will reinforces may but This sources spectrum, its variable of lenging. other hardening from monotonic quasar the birthing by such facilitated a surveys transient Distinguishing optical LSST. in the a identified with as be survey also could X-ray quasars soft birthing all-sky quencies, an viscosity, disks and circumbinary of density If sensitivity the surface delineate disk quasars. we high birthing rate, a merger such have SMBHB lumi- identifying the of observed for for spreading the proxy requirements using viscous a survey and as post-merger quasars curve, the of light for function resulting nosity model the and idealized disk an circumbinary Using the quasar. a of rct.W uln ceefretnigorapoc ohge post-Newtonian higher to eccen- approach and our axis extending semi-major for order. the scheme of a decay outline solu- the We Our to tricity. order. contributions PN spin 1.5 the to includes orbits tion quasi-eccentric binaries on hole orientations black spinning spin describing arbitrary waveforms Here with efficient produce parameterization equations. to Keplarian differential orbits generalized the coupled a of and of timescales system of However, separation the a evolve order. employ we to PN orbit requiring 2.5 high, per to is steps waveforms extended these many been implementing at recently directly decades of has cost two work computational almost the this for and available order, been PN have 2 in- orbits holes black quasi-eccentric spinning on by spiralling produced waveforms needed (PN) ingredients that post-Newtonian The compute important eccentricity. for to is account it that estimation models parameter waveform the consider we biasing To or eccentricity. signals significant with these detector missing wave avoid gravitational a of band the enter holes Abstract: waveforms theory; Newtonian Keywords: Eprint: Authors: orbits in quasi-eccentric binaries compact spinning for waveforms Computing http://arxiv.org/abs/1004.5322 ons,Ni . e,Je Shapiro Joey Key, J.; Neil Cornish, eea cnro aebe rpsdi hc h riso iayblack binary of orbits the which in proposed been have scenarios Several sr-hH;dt nlss rq;msiebnre fbakhls post- holes; black of binaries massive gr-qc; analysis; data astro-ph.HE; ∼ 10% y.I > If /yr. udmna hsc ihLISA with physics Fundamental 1% fteXryeiso srpoesdit pia fre- optical into reprocessed is emission X-ray the of WNotes GW

65 oe esfrG science GW for News & Notes Notes & News for GW science 66 WNotes GW itneacrc safnto frdhf o ore hr h esn os dom- noise effective lensing the the where for sources formula for fitting redshift inates. of a function provide a we as 2–3; accuracy of non-Gaussian distance factor the deter- a distance exploiting by this by improve typically that can mination, we show distribution, we magnification lensing Here the square of sources. nature the of by number the divided by the distribution limited of magnification is root sources lensing wave the uncer- gravitational limit of the of deviation the that ensemble standard an in believed to commonly even distance is the determination, It in distance tainty measurements. the candle in This standard uncertainty sight. perfect of of of line source the a along structures is magni- from lensing lensing lensing weak gravitational the by affected to however, due are, fication They extinction). are (and dust physics to fundamental insensitive by determined are luminosities intrinsic their because Abstract: Keywords: Eprint: Authors: the distribution of gravitational magnification non-Gaussianity the the using for diagram noise Hubble wave lensing weak the Reducing eial netgtdteeouino egn trcutr ihse lc holes. black seed with clusters nu- star have merging we of clusters, evolution star physical the nuclear the investigated of understand merically inter- to disappearance effort the in an for co-exist In responsible frequently mechanism galaxies. holes elliptical black revela- and recent massive bulges the mass and may mediate clusters clue star valuable nuclear A that events. the tion merger star in nuclear in dense preserved partake their not indeed why are explain do clusters to galaxies needs com- one intermediate-mass a then than and scenario, rather merger low- center hierarchical If their at cluster. hole black star massive pact a house to known are galaxies, Abstract: holes black supermassive Keywords: Eprint: black-hole to Authors: nuclear-cluster cores from galaxy dominated transition the On http://arxiv.org/abs/1004.3627 http://arxiv.org/abs/1004.3988 iaa hitpe . oz ailE;Cte,Curt Cutler, E.; Daniel Holz, M.; Christopher Hirata, ek,Kni rhm lse W. Alister Graham, Kenji; Bekki, rvttoa aesucsaeapoiigcsooia tnadcandle standard cosmological promising a are sources wave Gravitational in litclglxe,blee ob ul rmtemre flesser of merger the from built be to believed galaxies, elliptical Giant sr-hC;cosmology astro-ph.CO; sr-hC;atohsc;csooy asv iaiso lc holes; black of binaries massive cosmology; astrophysics; astro-ph.CO; udmna hsc ihLISA with physics Fundamental

etme ,2010 7, September oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 ovrec,i re oraietefl oeta fsadr iesa cosmological lensing as sirens the standard of of potential PDF full reliable probes. the and realize to results accurate order These an in prominent. obtaining convergence, less of become importance skewness the the Gaussian highlight of a resembles effects PDF the the and redshifts, closely, higher more At PDF. Gaussian the from that than a asrtoa n rcesfo wr ogatelpia galaxies. elliptical giant to dwarf from proceeds stel- nucleus-to-galaxy one the as in ratio reduction mass observed mechanism lar the this explain Moreover, to pathway merging. a galaxy provides during it destruction making how thus tidal and reveal density, to stellar susceptible we central clus- its mass, star lowering cluster wed significantly newly it, nuclear the expanding heats ter, host dynamically merger their a of during coalescence 1-5% binary their are that holes black Using igecsooia aaee,sc stemte density matter the as z such redshift parameter, at cosmological ( sirens single redshift standard a vs for distance that the find on We residuals diagram. the of Hubble distribution the and inferred fit- mean simultaneously their the by in ting parameters, lensing, cosmological from on scatter constraints larger derive We additional, distances. the in- as small Monte- well a including as use sirens, scatter, We standard trinsic of parameters. samples mock cosmological generate on to simulations depends Carlo whose and (PDF) skewed Lens- function highly distribution structure. is probability large-scale shape a by with lensing magnification gravitational introduces of ing presence the in sirens, unprecedented dard the with sources these of to be precision distance could luminosity (LISA), the Antenna determine Space Interferometer to Laser used the by detected be to expected Abstract: holes Keywords: Eprint: Authors: Distribution Magnification Lensing the the of of Importance Shape the Sirens: Standard with Cosmology h aaees h estvt oteapiueo h atrpwrspectrum, power matter the of amplitude the to sensitivity σ The parameters. the is w, state of equation hnteetoprmtr r osrie iutnosy h kwesyields skewness (by the improvement variance. simultaneously, enhanced same constrained the further are with a parameters PDF Gaussian two a these from When derived sensitivity the to compared 8 rmtecsooia eedneo h D ln,hwvr is however, alone, PDF the of dependence cosmological the from http://arxiv.org/abs/1004.3562 hn,Ce;Hia,Zoltan Haiman, Cien; Shang, h rvttoa ae Gs mte yisiaigbnr lc holes, black binary inspiraling by emitted (GWs) waves gravitational The sr-hC;atohsc;E oneprs asv iaiso black of binaries massive counterparts; EM astrophysics; astro-ph.CO; < ∼ 1% esuycsooia aaee osrit rmsc stan- such from constraints parameter cosmological study We . ∼ 50% udmna hsc ihLISA with physics Fundamental − 80% ihe hntesee esn D sused, is PDF lensing skewed the when tighter ∼ WNotes GW 120% ,oigt h orlto between correlation the to owing ), Ω m ∼ rtedr energy dark the or , ,tesniiiyto sensitivity the 1, ∼ 20% worse d L z) -

67 oe esfrG science GW for News & Notes Notes & News for GW science 68 WNotes GW o h asso h lc oe nerdt oe G at AGN power to inferred holes black account the can particular, of in masses and, the holes, of black for orders massive two more of to formation up earlier in is sults process latter at the rapid mass, but more with holes, scaling magnitude in similar black friction a massive follow dynamical most both the by hole for black favoring clumps time-scales central merging a the around of that disk decay out nuclear the orbital point for further We and sug- accretion hypothesis. and Bondi boost, this necessary of pro- We the tests supply possible cases. can gest all, clouds medium not squeezing intercloud but the and most, enhancing pressure in by turbulent magnitude alone. formation star pressure of of order by outflow-triggering an out that to gas pose up the by drive is can shortfall which The radiation observed in the energy obeying enough holes supply black insufficient: is condition oetmoutput, momentum Abstract: Keywords: Eprint: Authors: feedback AGN positive and winds Momentum-driven ore h mlydrltvsi etcpct n iethaigo lcrn nat- electrons temperature of electron heating low direct the to and infer lead capacity urally to heat relativistic us employed allows luminosity The technique unabsorbed source. super-resolution the X-Ray The estimate the and reveal center. presence and the observations in bright- Chandra surface source extensive X-Ray point the the fit from successfully We found limiting rate. profile and Bondi ness arcseconds of <1% several to at rate from gas accretion out the more Electron diffuses unbinding Energy inflow. radii, source accretion. the gravitational the These on inhibiting several for conditions injection. crucial boundary energy is the conduction and eliminate thermal injection partially mass to of help rates terms the are stars find individual from to winds considered Stellar conduction. and feeding self-consistent with Abstract: Keywords: Eprint: Authors: A* Sgr for Feeding Self-Consistent and Conduction with Model Inflow-Outflow http://arxiv.org/abs/1004.0702 http://arxiv.org/abs/1004.0857 ik o;Nse,Adi Nusser, Joe; Silk, hhrao,RmnV;Bgnf,FeeikK. Frederick Baganoff, V.; Roman Shcherbakov, epooeatotmeauerda no-uflwmdlna g A* Sgr near model inflow-outflow radial two-temperature a propose We oc aac osdrtosptalmto h aeo G radiation AGN of rate the on limit a put considerations balance Force crto ic;atop.O srpyis uemsiebakholes black supermassive astrophysics; astro-ph.CO; discs; accretion crto ic;atop.E srpyis aitru A* Sagittarius astrophysics; astro-ph.HE; discs; accretion L / c aal fdiigglci uewns eso htthis that show We superwinds. galactic driving of capable , udmna hsc ihLISA with physics Fundamental z & 10 . h obnto faceinadcaecnere- coalescence and accretion of combination The T e ≈ 4 · etme ,2010 7, September 10 10 L ertebakhl.Within hole. black the near K ≈ 4 · z 10 M ∼ • 32 6 − ergs . σ eaincannot relation

− 1

ftepoint the of oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 peei scmata xetdfo h ooa rmwr o h ai emission in radio region the for line radio- framework quasars. the coronal broad radio-quiet the not the of from or expected of whether as probe compact size can as the is frequencies sphere below higher at just Observations radii, object. gravitational this 800 of 0.04 about radius of a radius a with thus of source, and slope synchrotron pc, thick spectral optically rising an a implies gives slope GHz, The 8.5 at photometry earlier and accretion single a achieving radii. thus mag- all of measure, at order suitable rotation the model obtain Faraday and emission of thick agreement optically GHz nitude 86 fit we model same the Eprint: galaxies Authors: early-type of systems cluster globular holes the black and supermassive central between correlation A Keywords: Eprint: Authors: System Hole Black Binary Candidate a J1536+0441A, SDSS Quasar the of Localization Parsec-Scale asv lc oe(MH n h number the and mass (SMBH) the hole between black correlation massive power-law tight ably Abstract: holes black sive Keywords: temperature brightness mas 5400 focusing area NRAO J1536+0441A, of emission, SDSS The broad-line from kpc the emission for systems. region GHz of localization 8.4 optical types the for on both search as to used or subparsec was a emitter; VLBA with double-peaked system a (BBH) hole as black separation; binary a as interpreted recently systems, Abstract: holes black supermassive observations; 2 .Oesuc a eetd ihadaee fls hn16 a 85p)ada and pc) (8.5 mas 1.63 than less of diameter a with detected, was source One ). http://arxiv.org/abs/1004.0146 http://arxiv.org/abs/1004.0137 ukr,Ades rmie Scott Tremaine, Andreas; Burkert, A. Laor, M.; J. Wrobel, h ai-ue usrSS 13+41 hw w ra-ieemission broad-line two shows J1536+0441A SDSS quasar radio-quiet The litcl etclr n al-yesia aaisso remark- a show galaxies spiral early-type and lenticular, Elliptical, sr-hG;atop.E srpyis asv iaiso lc holes; black of binaries massive astrophysics; astro-ph.HE; astro-ph.GA; sr-hC;atohsc;goua lses bevtos supermas- observations; clusters; globular astrophysics; astro-ph.CO; T b ∼ 5 x 10 T 10 udmna hsc ihLISA with physics Fundamental b .Teipidrdoshr trs rm 12Gzhas GHz 31.2 frame rest at radio-sphere implied The K. > 1 . 2 x 10 7 .NwNA L htmtya 25GHz, 22.5 at photometry VLA NRAO New K. WNotes GW N GC fgoua clusters: globular of M BH ftercnrlsuper- central their of α 0.35+/-0.08. = M 2 BH (0.15 =

69 oe esfrG science GW for News & Notes Notes & News for GW science 70 WNotes GW nalmtdsml f1 aais hsrlto per ob etrpeitrof predictor better Based a be clusters. to globular the appears the than relation of dex) this 0.2 mass scatter galaxies, (rms total 13 mass the SMBH of as sample same limited the a is on mass SMBH the tion timesN m re em nteP ria nry hs osrit ol epi constructing in help could constraints These energy. orbital 5PN PN and the metric, 4PN effective in EOB (3) terms the and order (1) of templates, knowledge inspiral-merger-ringdown our phenomenological constrain the to (2) how used be consider can also ISCO, the I computations relativity of numerical with methods. combined self- PN shift, ISCO conservative standard suggest self-force conservative incorporate than study accurately calibration) this more of effects of absence force test-particle results the conservative The (in the not incorporating dynamics—does exactly performed. methods approach—while also PN EOB is of the comparison that ISCO A equal-mass the reproduces the resummation. method gauge- any with This without the (2003). limit from Iyer test-particle found currently-known and exact Blanchet is the of agreement on condition best ISCO only invariant the based dynamics, methods How- conservative uncalibrated simulations. 3PN-order considers relativity effective- numerical one from to if found fit is ever, are result that exact calculations the (EOB) with one-body agreement "non- best both limit The include test-particle construction). the These reproduce by latter shift methods. (the approaches ISCO PN-based "resummed" exact known and resummed" this all Here nearly approx- results ISCO. with with concrete the compared comparison first is of of the computations point of (PN) exact an one post-Newtonian provides imate is and This from program, self-force arises test-particle. the that orbiting of self-force an conservative the of to finite-mass due the (ISCO) orbit circular stable most Abstract: waveforms theory; Newtonian Keywords: Eprint: Authors: methods based post-Newtonian- multiple with sta- comparison innermost orbit: circular the ble to correction self-force Conservative recent with associated are mergers. populations major cluster globular large and masses black-hole high with galaxies that fact frequency the specific reflects cluster scatter globular small The sigma. dispersion velocity hnepce rmthe from expected than http://arxiv.org/abs/1008.4622 GC 1 aaa Marc Favata, arde]Brc n aohv eetycmue h hf fteinner- the of shift the computed recently have Sago and Barack [abridged] . 11 + sr-hH;Efcieoebd;ER;gnrlrltvt;g-c post- gr-qc; relativity; general EMRI; body; one Effective astro-ph.HE; / − 0 . 04 with M m udmna hsc ihLISA with physics Fundamental BH = − 1 . σ 3 eain osbeepaaini htbt large both that is explanation possible A relation. × S 10 N 5 edt abrSBsta r oemassive more are that SMBHs harbor to tend oa ass hs oago approxima- good a to Thus, masses. solar M BH −

σ etme ,2010 7, September eainbtenSB asand mass SMBH between relation oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 etrgaiainlwv epae.Lsl,Isgetanwmto ocalibrate to cal- method numerical-relativity "low-cost" new using culations. a templates inspiral suggest in I PN-terms Lastly, unknown templates. gravitational-wave better in o cieGlxe.I ehdlg n eut of Rela- Results Study and Scaling Pilot Methodology Mass I. Hole Galaxies. Active Black for the tions of Baseline Local A Keywords: Eprint: Authors: in Galaxies Connection Hole Black Cluster/Central Globular The Eprint: A. Matthew Malkan, Hak; Authors: either in +-0.2 of scatter "cosmic" or intrinsic an have also must log the galaxies by S defined relation and mean E the that find we uncertainty, measurement in servational scatter large showing trend, clear Tremaine to & proportion Burkert direct by cisely discussed that sample find original the we as (2010), large as twice galaxies, 33 ( galaxy a Abstract: holes black sive htruhy1%o h aaisi u ape(n ,oeS n w 0 deviate S0) two relation. their mean and that the S, sense by one predicted the be E, in would (one all than sample trend, our main the in note from galaxies we strongly the Lastly, of formation. 10% for roughly conditions that merging, high-density hierarchical extremely of because require epoch correlated main both the closely and subsystems during be redshift galaxy high may at of system) originated types cluster both they globular two and these hole that black suggest (central We frequency. specific cluster N GC http://arxiv.org/abs/1008.4748 http://arxiv.org/abs/1008.4602 rlog or ars rthnL . ars ila E. William Harris, H.; L. Gretchen Harris, N enr,Vrh ioa ue,MthwW;Te,Tmao o,Jong- Woo, Tommaso; Treu, W.; Matthew Auger, Nicola; Vardha Bennert, eepoeterlto ewe h oa lblrcutrpplto in population cluster globular total the between relation the explore We GC sr-hC;atop.A srpyis lblrcutr;supermas- clusters; globular astrophysics; astro-ph.GA; astro-ph.CO; M n h h aso t eta lc oe( hole black central its of mass the the and ) BH h eiul rmti orlto hwn rn ihglobular with trend no show correlation this from residuals The . N GC udmna hsc ihLISA with physics Fundamental o litcladsia aaisicessi lotpre- almost in increases galaxies spiral and elliptical for M BH h 0tp aaisb otatd o olwa follow not do contrast by galaxies S0-type The . M BH WNotes GW tagiven a at N GC M fe conigfrob- for accounting After . M BH BH sa es 0 smaller 10x least at is .Uigasml of sample a Using ).

71 oe esfrG science GW for News & Notes Notes & News for GW science 72 WNotes GW ieglxe.I h etppr ftesre ewl uniytesaigrelations, scaling the quantify will we of series inac- sample and the full active of of the local papers relations other exploiting next scaling of the those MBH In with the scatter galaxies. Third, and tive slope in percent. agree few sample a pilot our within can region, to lines, CaHK emission accurate and the results continuum and powerlaw give AGN emission, the FeII by for swamped dis- often corrected stellar-velocity although region, red- determine MgIb higher to cleanest at the the relation both is MBH-sigma persions, region the CaT in the seen while offset Second, the shifts. However, explain morphology. cannot host-galaxy bias and a depend- contamination, such biased, AGN be size, can galaxies) aperture distant on from ing data unresolved (e.g. or spectra spectra aperture fiber from SDSS determined follow- dispersions stellar-velocity the First, find results. We ing relations: scaling MBH-M(sph,dyn). MBH MBH-M(sph,*), four study MBH-L(sph), to MBH-sigma, us the allows of re- imaging Combining width and luminosity. spectroscopy the AGN from developed from 5100A sults free newly estimated host-galaxy are the a and masses line using BH emission Hbeta images, addi- analysis. SDSS In multi-band joint on triplet). for photometry CaII code surface and perform triplet, we MgIb spa- tion, CaH&K, of (including level from regions curves unprecedented spectral rotation an and three profiles with de- dispersion We galaxy stellar-velocity deriving host properties. resolution, ( the tial host-galaxy of SDSS and kinematics (MBH) the stellar mass from termine hole selected black galaxies between relations active the local 25 of ple Abstract: Keywords: gigfo oe-a oiae otemldmntd sntascae iha with associated X- not the is that 2008 dominated) and find thermal 2004 to we of dominated results, observations power-law published XMM-Newton from previously two (going the to between Contrary change spectral kpc. ray 3 times to few 1.5 with a star about an neutron about with foreground a of consistent with We luminosity equally or state, are a high hole. properties a black timing in hole and intermediate-mass black spectral intermediate-mass an X-ray as the identification that its show for evidence the amine Abstract: observations Keywords: Eprint: Authors: or hole black star? intermediate-mass neutron foreground HLX1: of study X-ray http://arxiv.org/abs/1008.3382 oi,Rbro apei ua ae iva u Kinwah Wu, Silvia; Zane, Luca; Zampieri, Roberto; Soria, epeethg-ult ekLI ogltsetocp fapltsam- pilot a of spectroscopy longslit Keck/LRIS high-quality present We er-sesteXMNwo n wf bevtoso L1 oex- to HLX1, of observations Swift and XMM-Newton the re-assess We sr-hC;osrain;sprasv lc holes black supermassive observations; astro-ph.CO; sr-hC;atop.E srpyis nemdaems lc holes; black intermediate-mass astrophysics; astro-ph.HE; astro-ph.CO; udmna hsc ihLISA with physics Fundamental ∼ 0 objects. 100 10 32 erg/s ∼ etme ,2010 7, September 10 − 6 L Edd 0 oae tadsac of distance a at located , . 02 < z 10 7 M

ostudy to ) oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 IBs n hi xsec ssilhaiydsue,s hywl epretfril- for perfect hunter Holes be hole Black will black they a Mass by so Intermediate faced disputed, challenges named heavily observational are still the lustrating size is existence this 10000 their to of and 100 holes from (IMBHs) Black approximately masses, will black-hole masses. I of questions, solar claim range these they particular answer when To a mean on existence? re- really their focus astronomers theoretical of do of evidence What wealth observational have a exist? to really yielding they deal, do great But a sults. studied been have they equations Abstract: dynamics stellar lectures; of notes consistent is that way a in but Swift, by dominant scenario. seen more either outburst becomes with 2009 component the thermal during The hotter) (and luminosity. X-ray the in change rmabakhl spsil.()Teei os-aldinrotsal iclrorbit. circular stable innermost so-called no is radii There Schwarzschild (3) 2.25 possible. and is 1.5 hole between black precesses. distance a and a from elliptical at thus orbit is circular "circular" the and unstable most eccentricity An in The nonzero (2) relativity but possible. small general not a to is have orbit according must circular orbit field stable gravitational A a (1) in metric: Schwarzschild particle a for orbit lar Abstract: Keywords: Eprint: Authors: Rela- General to According tivity? Possible Orbit Circular a Is Keywords: Eprint: Authors: IMBHs GCs on in notes lecture 2010 School Hole Black Croatian http://arxiv.org/abs/1008.4477 http://arxiv.org/abs/1008.3553 ie .T;Kee,David Kuebel, T.; F. Hioe, Mario Pasquato, lc oe r acntn bet.A ls fsltost h Einstein the to solutions of class a As objects. fascinating are holes Black h olwn eut r rsne ocrigtepsiiiyo circu- a of possibility the concerning presented are results following The MI eea eaiiy gr-qc relativity; general EMRI; sr-hG;goua lses rq;itreit-asbakholes; black intermediate-mass gr-qc; clusters; globular astro-ph.GA; udmna hsc ihLISA with physics Fundamental WNotes GW

73 oe esfrG science GW for News & Notes Notes & News for GW science 74 WNotes GW egr.Oraayi ugssta h iayeouino ardsupermassive paired of evolution binary masses of to the (both nuclei that holes in black suggests activity radio analysis the of for Our relationship implications the (2) mergers. (3) holes, and post- systems, black cos- for "stalled" two implications a of the (1) with possibility of of compared centralisation terms is for in result timescales interpreted This merger and nucleus. model double rate merger a mological as detected Only was nuclei. map- source radio-emitting index double one spectral resolved, radio spatially a targets which using technique holes ping black supermassive binary for searched we Abstract: Keywords: Eprint: Holes Authors: Black Supermassive Binary of Census Radio A emfrtesit eas eiea xrplto t nnt ais oml o the for formula radius) infinite damping (to runs, extrapolation variable an a numerical derive with also full We approach shift. those punctures the moving perform for the term gravi- to of the order gauge the when In adapted radians 0.2/M. we <0.05 is errors frequency with wave highest accuracies tational The dif- phase from resolutions. reach difference q=1/15 finite runs simu- and different resolution numerical q=1/10 for ratios full and mass of separations with initial series black-hole- ferent holes a black (IMR) perform nonspinning We ratio of mergers. mass lations and intermediate inspirals from (BHB) radiation binary gravitational the pute Abstract: waveforms relativity; numerical holes; black of Keywords: Eprint: Manuela Authors: techniques perturbative and numerical intertwin- ing binaries: hole black Intermediate-mass-ratio correlated is holes kpc. black 2.5 rela- supermassive of the paired separations that orbital between stalled evidence within emission of circumstantial radio excess see of We an state for tive separations. evidence small no at show for systems data radius The binary stalling purported pairs. the hole within to black cores supermassive stellar galactic of merging the from http://arxiv.org/abs/1008.4360 http://arxiv.org/abs/1008.4382 uk-plo,Sarah Burke-Spolaor, edsrb ndti ulnmrcladprubtv ehiust com- to techniques perturbative and numerical full detail in describe We sn rhvlVB aafr31 ai-uiosatv aatcnuclei, galactic active radio-luminous 3114 for data VLBI archival Using oso alsO;Nkn,Hryk;Zohwr oe;Campanelli, Yosef; Zlochower, Hiroyuki; Nakano, O.; Carlos Lousto, sr-hC;atohsc;msiebnre fbakhls observations holes; black of binaries massive astrophysics; astro-ph.CO; sr-hC;atop.A sr-hH;g-c MI asv binaries massive IMRI; gr-qc; astro-ph.HE; astro-ph.GA; astro-ph.CO; udmna hsc ihLISA with physics Fundamental geqslant 10 8 M

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etme ,2010 7, September oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 ics h oeigo h ulisia n egrbsdo obndmatching combined trajectories. a Geodesic on and based before Numerical, We merger Full modes. orbits and Post-Newtonian, three inspiral 8 of all full for includes the 99.7% of which near modeling overlaps case, the obtain discuss q=1/10 we case, the 98.3% q=1/15 in and the For modes, mode merger. (3,3) (2,1) and nonleading (l,m)=(2,2) perturbative the spins leading and for final the numerical the for full Including 99.5% comparing reaching when a/M<0.3. frequen-waveforms, functions spins (QNM) for overlap mode agreement large the quasinormal good improves the the find of computing we spins by where intrinsic it cies, small validate account and into hole, take black to formalism extend then perturbative We of this terms formalism. source perturbations the Schwarzschild full in Regge-Wheller-Zerilli the gauge, the use Schwarzschild we the evolutions into perturbative transformed the tracks, For numerical radius. finite at extracted waveform o crtn 0 fteds asaei h ag 3-4 y,dpnigon depending Myr, 130-540 range the in are required mass timescales disk The the disk parameters. of initial model the 50% on of accreting half dependent for a weakly about result capture a seeds mass, that indicate simulations on present based The is mesh. code staggered a numerical on to The algorithm according second-order, upwind of Leer itself. Van method difference the both disk finite a the contributions using from formalism, includes Eulerian and a potential object gravitational central the the axi- from which an in for numerically disk solved symmetric were equations hydrodynamic time-dependent The evo- disk seeds. accretion of the growth of the aspects mech- of particular transport and these momentum lution to angular addressed the like is on parameters or paper seed on This the depend anism. or quantities disk these the of how mass as timescale initial related well the the as and questions, object central open the still by are captured disk the of fraction mass coalescences The by and/or disk of circumnuclear growth a the episodes. by from merger formed the during mass are of accreting objects majority by exotic the these either of that seeds consensus centre a the is in There present galaxies. probably are holes black Supermassive Abstract: Keywords: Eprint: Authors: accretion by disks fed holes black supermassive of growth The http://arxiv.org/abs/1008.4150 rio .A otsns ahc,J .d Freitas de A. J. Pacheco, Montesinos; A. M. Armijo, crto ic;atop.O omlg;sprasv lc holes black supermassive cosmology; astro-ph.CO; discs; accretion udmna hsc ihLISA with physics Fundamental WNotes GW

75 oe esfrG science GW for News & Notes Notes & News for GW science 76 WNotes GW between aaiswoerneo uioiiscrepnst eta lc oems ( mass hole black central a to corresponds luminosities of range whose galaxies Clusters Archival Galaxy an of from Survey 1689 X-ray Abell in Flare Disruption Tidal A unified the to support structures additional these an of representing presence AGNs, the of model. regions for central explanation the natural in a offering bright of develops, presence etry the explain to z permit at quasars timescales These parameters. adopted the uiga pial rgtflr frdain epeittesetaadspectral and spectra the predict pro- We BH, the radiation. from of away blown flare subsequently bright is optically gas an this ducing of fraction A rate. dington MBH Abstract: Keywords: Eprint: of Disruption Authors: Tidal Holes Black Massive the by Stars of Signatures Spectroscopic of rate disruption tidal a estimate we cluster, the 1 of studies factor existing a by by determined vary to observed is s flare The 1689. of Abell ex- in resulting using We clusters J131122.15-012345.6 the galaxy SDSS itself. of of hole portion survey archival black a expected ongoing the and an dra be onto of disrupted circumstances results back is first falls most it the debris amine under as stellar radiation can shock-heated of galaxy of flare stream a giant of a center emit to the at hole black Abstract: holes black sive Keywords: Eprint: Authors: − . 2 1 & × n oei sabakoywith blackbody a as emit to and and 30 10 lesssim − http://arxiv.org/abs/1008.4131 http://arxiv.org/abs/1008.4140 XMM-Newton vra es er,t aemaximum have to years, 2 least at over 4 10 tub,LnaE;Qaar,Eliot Quataert, E.; Linda Strubbe, Michael Eracleous, P.; Melville Ulmer, Peter; Maksym, uigtetdldsuto fasa yamsiebakhl B)o mass of (BH) hole black massive a by star a of disruption tidal the During galaxy hoysget htasa aigacoepsaeb supermassive a by passage close a making star a that suggests Theory 6 sr-hC;atohsc;E oneprs uemsiebakholes black supermassive counterparts; EM astrophysics; astro-ph.CO; sr-hH;atohsc;E oneprs bevtos supermas- observations; counterparts; EM astrophysics; astro-ph.HE; ∼ 10 and ..Mroe,a h n fteds vlto,a“ou-ie geom- “torus-like" a evolution, disk the of end the at Moreover, 6.5. 7 M − 10

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• ) oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 lc oeo oeta 0 Msun. 500 than mass more intermediate finding of accreting an hole This containing lu- black it maximum for 243-49. extreme case the ESO the strengthening confirming of and 243-49, minosity that ESO with inside identified HLX-1 recently consistent places the redshift definitively for object. a line the as- emission at of definitive Halpha nature counterpart the the a optical of confirm so detection to kpc, order the 2.5 report in crucial we only Here is quiescent of galaxy a distance host be Galactic the could with a ultra- HLX-1 sociation at that other binary claimed X-ray of been star number or recently neutron galaxies a has active However, luminosity background It the as sources. value). identified (assuming foreground later Eddington Msun been the 500 have sources above of X-ray 10 excess luminous in of intermedi- mass accreting factor an a a implying with is as hole interpreted black been mass has ate and hole, black Msun 20 events. disruption tidal discovering transient for optical potential help their should on predictions capitalize Our surveys Telescope. Space Hubble adaptive the re- with or imaging be follow-up optics can high-resolution using contamination level Supernova manageable but a galaxies. to rate red duced comparable pre-selecting a by z at excluded at occur be supernovae events can II disruption Type tidal Nuclear than surveys. common ground-based are more supernovae magnitude optical Ia Type of in nuclear orders that confusion estimate two of we source events: significant disruption tidal a for are surveys nuclei UV galactic lasting at in VI), strongest supernovae O and while, alpha, (0.01-0.1c), Ly IV, broad strongly C very are (e.g., galaxy, wavelengths that host lines the absorption to this show relative outside will gas blueshifted spectrum photoionized The the on photosphere. focusing outflow’s events, disruption tidal of evolution h otglx itneo 5Mc h aiu bevd02-1 e luminos- keV 10 - is 0.2 luminosity observed This maximum the erg/s. At 1.2E42 Mpc, 243-49. is 95 ESO ity of galaxy distance the galaxy with host source, the X-ray ultra-luminous brightest the HLX-1, Abstract: observations holes; black mass Keywords: Eprint: Olivier Godet, Didier; Barret, J.; Thomas Maccarone, Authors: the with 243-49 Association ESO Can- its Galaxy Hole of Confirmation Black Mass HLX-1: Intermediate didate the for Redshift A http://arxiv.org/abs/1008.4125 nti etrw eotasetocpccnraino h soito of association the of confirmation spectroscopic a report we Letter this In irea la;Frel enA;Wb,NtleA;Srilt Mathieu; Servillat, A.; Natalie Webb, A.; Sean Farrell, Klaas; Wiersema, sr-hC;atop.A sr-hH;atohsc;IR;intermediate- IMRI; astrophysics; astro-ph.HE; astro-ph.GA; astro-ph.CO; udmna hsc ihLISA with physics Fundamental ∼ WNotes GW 0 ie bv h digo ii o a for limit Eddington the above times 400 ∼ ot o a for month 1 10 6 M

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77 oe esfrG science GW for News & Notes Notes & News for GW science 78 WNotes GW fofcnrdANi ikdwti a-ihdss–u oafwprcn fthe of cent few per a few of timescales a on to variable up highly – are detection discs and the – gas-rich for rate within high accretion kicked favourably Eddington are if of galaxies rates AGN accretion simulated off-centred Bondi-Hoyle-Lyttleton the our of The to in return BHs delay. fast recoiling significant a a the both facilitate as can well and sur- as in complex the centre stars with general BHs and in kicked is gas of medium of interaction rounding dynamical distribution the However, and the BHs centre. affecting recoiled galactic besides of the orbit timescale, discs. the return stellar modify purely their strongly for can hence than feedback timescale and shorter accretion much recoiled a BH allows on disc Also, centre gaseous the massive to a return of to presence BHs the that hydrodynami- find high-resolution We of means simulations. by cal galaxies gas-rich massive in (BHs) holes Abstract: kicks/recoil Keywords: Eprint: Authors: galaxies rich gas hy- of simulations in drodynamical holes black supermassive of recoils Gravitational betwt tla asi iclrobti h qaoilpaeo supermassive a of plane equatorial the in orbit circular a in mass stellar with object Abstract: Keywords: Eprint: Authors: Hole Black Kerr Supermassive a Ob- circling Compact ject Spinning a from Radiations Gravitational occur.[Abridged] redshifts, to expected high is at recoils galaxies BH of massive bulk from the escape where epoch to supermassive the able result, is be which a As rarely only central baryons. the of should in concentration BHs steeply dissipative remnants falls the that the to mas- potential due as clumpy gravitational regions, well the a as that exhibit observations, mergers, is than high-redshift gas-rich models kicks of recent numerical recoil by our to suggested of sensitive result discs more simu- generic sive being A to compared mass mass. relationships BH bulge galaxy the the host with – kicks, recoils mass gravitational without BH that lations the find in we scatter galaxies, the gas-rich increase of simulations merger major In http://arxiv.org/abs/1008.3324 http://arxiv.org/abs/1008.3313 iak,Dbr;Srne,Vle;Henl,Martin Haehnelt, Volker; Springel, Debora; Sijacki, a,Wen-Biao Han, h rvttoa ae n nryrdain rmasinn compact spinning a from radiations energy and waves gravitational The esuyteeouino rvttoal eoldsprasv black supermassive recoiled gravitationally of evolution the study We MI eea eaiiy rq;spin gr-qc; relativity; general EMRI; crto ic;atop.O Mcutrat;gaiainlrecoil; gravitational counterparts; EM astro-ph.CO; discs; accretion udmna hsc ihLISA with physics Fundamental etme ,2010 7, September 10

7

yrs. oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 iaiswith binaries particle. is non-spinning particle the spinning than one. extreme bigger non-spinning the the much of than energy more binging much maximum is the hole consequently, black And near Kerr radiation extreme with energy the comparing the of the “negative” value, horizon the into for spin extreme inspiral shorter for and particle Especially, spin of particle. “positive” time non-spinning for the in- longer that during is find From accumulation We hole wave-phase black function. particle. the the quadratic estimate of a we process between like spiralling spin, relation looks to the spin due And and shift horizon) frequency enlarged. and be infinity infinity spin), (both spin to (“positive” fluxes anti-direction direc- fluxes For momentum infinity. the energy angular to the when orbitally radiate which the (“negative”), that fluxes as energy clear the same is decrease as can It is spin axes detections. spin of wave production tion gravitational waveform-template indicate in upcoming results considered calculation the be should The for body small detail. of in energy spin on discussed the acts that is spin the fluxes how moment effect The angular paper. and this in investigated are hole black Kerr et fN aeom uhta h nlhbi aeom etti require- this meet waveforms require- hybrid with length final binaries the the nonspinning of that question considering such the ment, address waveforms We below NR is 0.97). of error about ments factor mismatch fitting their a if are (i.e., detection waveforms 3% Hybrid GW hybrid. for the accurate in increasing included sufficiently by are hy- reduced considered that in be cycles GW can source NR and error of contribution, dominant number search the PN The GW the from pipelines. for arises search models waveforms GW brid phenomenological of tests some for of and construction templates, the to waveforms central Hybrid waveforms. are “hybrid” and create (PN) to post-Newtonian results (NR) connect numerical-relativity to is systems black-hole-binary from waveforms Abstract: waveforms theory; Newtonian Keywords: Eprint: Authors: waveforms numerical-relativity for requirements Length ein fprmtrsaefrwihtelatnme fcce ilb needed. be will cycles of number least the which for space parameter of regions ltosms oti ewe he i h qa-asnnpnigcs)adten and case) nonspinning equal-mass the (in (the three between contain must ulations χ = http://arxiv.org/abs/1008.2961 0 anm ak ua aca he rn;Aih P. Ajith, Frank; Ohme, Sascha; Husa, Mark; Hannam, . n a opouecmlt nprlmre-igongravitational inspiral-merger-ringdown complete produce to way One 5 ae risbfr egr u hr sas vdneta hs r the are these that evidence also is there but merger, before orbits case) rq;msiebnre fbakhls ueia eaiiy post- relativity; numerical holes; black of binaries massive gr-qc; χ = S i / M i 2 ∈ udmna hsc ihLISA with physics Fundamental [ − 0 . 5 , 0 . 5] ecnld htfrtecssw td sim- study we cases the for that conclude We . WNotes GW q = M 2 / M 1 ∈ [1 , 4] n equal-mass and

79 oe esfrG science GW for News & Notes Notes & News for GW science 80 WNotes GW Abstract: Keywords: Eprint: Authors: of case the OJ287 jets: blazar optical in stability and Variability Ssi aetp ik n nshriascudhv sebe rmmigrating from assembled have could spheroidals grows in NSC and the the that disks find which late-type and dissolution at in and rates rate NSCs migration formation cluster The cluster model We becomes empirical times. from center. and dissolution estimated and the galaxy be can reaches the clusters it tidal of young accreting galactic if center by the NSC the and toward the mass radially in initial migrates integrated its cluster by The determined gravita- period field. remains a young, galaxy A over star-forming clusters. bound isolated in tionally an form stars con- in of the embedded majority in a cluster inevitable which mass-losing in is formation NSCs star of normal formation of text The galaxies. spheroidal and type-disk Abstract: Keywords: Eprint: Authors: Formation Star Clustered from Clusters Star Nuclear of intervals regular at bursts htcagsi h e antcfil rv h eua outbursts. regular the drive field observations. magnetic assumption the jet the on the explain based in is fully changes that to OJ287 that understanding able to is approach new none models a that possible bole suggest We find on black we constraint binary observations, new proposed available the a all of as Combining findings related models. our tightly hole magnetic seem use black field We jet binary magnetic the jet bursts. of optical double-peaked the reorientation the in a to changes has indicating that it find plane that also find Stokes polariza- We and the field. optical core in polarization historical optical swing Using the a of jet. showed evolution the the that trace to we indicates parallel data, polarization oriented tion optical is The in field core. component magnetic polarization stable the optical a the find We jet: optical occurred. the outburst black double-peaked binary during latest supermassive 2005-2009, the from close data which a monitoring host photopolarimetric optical might present OJ287 We that hole. suggested been has it ior, http://arxiv.org/abs/1008.2986 http://arxiv.org/abs/1008.3082 ilot,C;Nlsn . ed,J;Prio T. Pursimo, J.; Heidt, K.; Nilsson, C.; Villforth, gra,Mgan ioalei,Milos Milosavljevic, Meghann; Agarwal, J8 saB a beta esitz036ta a hw double-peaked shown has that z=0.306 redshift at object Lac BL a is OJ287 htmtial itntncersa lses(Ss r omni late- in common are (NSCs) clusters star nuclear distinct Photometrically sr-hC;atohsc;msiebnre fbakhls observations holes; black of binaries massive astrophysics; astro-ph.CO; sr-hC;atop.A srpyis MI tla dynamics stellar IMRI; astrophysics; astro-ph.GA; astro-ph.CO; udmna hsc ihLISA with physics Fundamental ∼ 2y uigtelast the during yr 12 etme ,2010 7, September

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0y.Det hsbehav- this to Due yr. 40 oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 n h rcino lsessfeigpop islto.W ne rnainmass truncation infer ICMF We the dissolution. of prompt scale of suffering mass scales clusters truncation ob- the of with constrain fraction Comparison to the used way. and be this can assembles masses mass disks, NSC in pseudobulge served phenomenon the pseudobulge of the all to not related galaxy. be though outer can the excess of the law that Sersic) suggest extended We (or more exponential spatially inward-extrapolated a observed the by the over surrounded are excess with NSCs consistent final are cluster the generically, masses initial but the NSC values, of resulting truncation The high-mass of (ICMF). the mass function to stellar mass sensitive the is of fraction fraction this small galaxy; a the contains nucleus stellar resulting The clusters. tcatct nbt h o n ne ogai ueobtfamilies. orbit tube of long-axis levels inner high matter and the dark box to the due and both exist galaxies to in unlikely stochasticity elliptical are speeds triaxial pattern equilibrium intermediate with but rapidly halos very bars, or axis. rotating fast slowly short like be the central either rotating (with could about halos holes) matter circulate black dark supermassive and and and loop- galaxies cusps bars, retrograde triaxial 3-D stable stable that of in implies family analysis orbits Our new resemble a box- which to bars) orbits, transition triaxial of like sudden that a to undergo (close orbits speeds the like pattern in in highest increase decrease the corresponding sharp At a a and variety. triaxi- also tubes retrograde maintaining short-axis is prograde for there of important increases fraction most speed overall are pattern the As that families chaotic. orbit highly two Gyr are .2 the ality periods Gyr, rotation long-axis 5 pattern < inner for Tp Thus as center. < destabilizing forces, well coriolis the the as into from driven orbits arises are that and box doubling" "envelope resonant the by the pattern destabilized are intermediate of tubes At fraction space. stable. significant largely configuration are a families in speeds orbit associated surfaces all are rotation dimensional figure triaxiality) two slow maintaining For occupy for which (vital such resonances orbits In with box holes. black regular supermassive most central with galaxies, potentials triaxial realistic of family Abstract: Keywords: Eprint: Authors: Figure with Galaxies Triaxial Rotation of Structure Orbital The http://arxiv.org/abs/1008.2753 ∼ ebl lxT;Vlui oia ert,David Merritt, Monica; Valluri, T.; Alex Deibel, esre h rpriso l ri aiisi h oaigfaeo a of frame rotating the in families orbit all of properties the survey We 10 sr-hG;atohsc;ER;selrdynamics stellar EMRI; astrophysics; astro-ph.GA; 5 M

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81 oe esfrG science GW for News & Notes Notes & News for GW science 82 WNotes GW fmauigvi h otx ftehn o MH ngoua clusters. globular in IMBHs for hunt the of usefulness context the the on doubts in serious v casts measuring and of IMBH central a of signature unequivocal (Sigma Abstract: dynamics stellar N-body; holes; black Keywords: Eprint: Authors: surface- the clusters globular in of cusps profile brightness shallow of presence Widespread ea ihcutr,js si h aefrbih -a ore ngeneral. in sources X-ray bright for is case and there the bright is that in as favored find just is and clusters, formation rich candidates, binary metal X-ray binary source hole X-ray black this hole that of black evidence cluster suggestive strong host the other of six properties the the accreting and consider single We a from hole. also expected black spectrum be mass would X-ray stellar what source’s with The consistent strong manner hole. a a black in is cluster evolves and star, globular a neutron a has single being a and for for 4, candidate luminosity of Eddington factor the a than least more at cantly least by varies at that of source luminosity a peak find we galaxy, the NGC of galaxy vations elliptical the in cluster ular Abstract: observations holes; Keywords: Eprint: L. ine 4472 NGC Authors: in hole black cluster globular new A cusps, when steeper even to 0.3 transition IMBH an without − clusters Post-core-collapse phases. 0 . 7 < ∼ ∼ http://arxiv.org/abs/1008.2896 http://arxiv.org/abs/1008.2771 eprn,Erc;Tet,Michele Trenti, Enrico; Vesperini, acrn,Toa . ud,Aua;Zp,SehnE;Roe Kather- Rhode, E.; Stephen Zepf, Arunav; Kundu, J.; Thomas Maccarone, edsusCXOU discuss We ufc rgtespolso lblrcutr ihsalwcnrlcusps central shallow with clusters globular of profiles brightness Surface v R sr-hC;atop.E srpyis MI nemdaems black intermediate-mass IMRI; astrophysics; astro-ph.HE; astro-ph.CO; sr-hG;atohsc;goua lses MI intermediate-mass IMRI; clusters; globular astrophysics; astro-ph.GA; v < with − ∼ . − 0 0 − . . 0 4 4 . nyi h rmrilbnr rcini eysmall, very is fraction binary primordial the if only , vrl u nlsssosta hlo upi o an not is cusp shallow a that shows analysis our Overall . 3 < udmna hsc ihLISA with physics Fundamental ∼ 2 ∼ × 291+774 e lc oecniaei glob- a in candidate hole black new a 1229410+075744, v 10 − ∼ 39 rssc ssc,tesuc aisb signifi- by varies source the such, As ergs/sec. 0 . 3 ∼ ntepecr-olpeadcore-collapse and pre-core-collapse the in 42 ycmaigtoCadaobser- Chandra two comparing By 4472. etme ,2010 7, September f bin

- oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 yaia apn em o ymtyseigshift symmetry-seeking conditions for terms damping Dynamical Keywords: Eprint: black Authors: onto accretion holes of characteristics Observational when useful be ratios. therefore mass could small and very hole with size black binaries coordinate larger simulating the the in of variations horizon the apparent black- reduces the binary also of simulations the condition our of gauge masses in Our and instabilities system. positions of hole individual tuning free the special is to for adapts which dynamically need term and the damping removes shift choice a an of this provides solution that and the show and We variable dynamical which equation. a in be evolution to condition promoted gauge stable is novel long-term constant a damping ensure present the to We parameters binaries. its unequal-mass of re- of tuning evolutions condition non-trivial shift time, and "Gamma-driver" careful same standard a the the quires non-vacuum At that and emerged masses. vacuum has comparable in evidence recent with both binaries used simulating successfully and when been lapse the spacetimes have both these for and decade last shift the the over developed been well- have of conditions number studied A binaries. compact inspiralling of simulations numerical-relativity Abstract: Keywords: Eprint: Authors: hsrdainwt atrcnrsl npooeeti bopinado reflection. of and/or interaction absorption photo-electric The in respectively. result can components, matter spectral with disc radiation and this producing tail holes, black X-ray accreting hard radiation for blackbody the mechanisms and radiation scattering predominant Compton two outline sur- I the complete such, as field. a As the representing in than done sources. rather work reading, powered of get start vey accretion to to study place subject, a to in give used references starting the tools just fundamental those the especially of students, hold help to designed are They Abstract: holes black sive http://arxiv.org/abs/1008.2212 http://arxiv.org/abs/1008.2287 oe Chris Done, Philipp Mösta, Ian; Hinder, Luciano; Rezzolla, Daniela; Alic, hs oe eutdfo eiso etrsa h A itrschool. winter IAC the at lectures of series a from resulted notes These utbeguecniin r udmna o tbeadaccurate and stable for fundamental are conditions gauge Suitable rq;msiebnre fbakhls ueia relativity numerical holes; black of binaries massive gr-qc; crto ic;atop.E srpyis oe flcue;supermas- lectures; of notes astrophysics; astro-ph.HE; discs; accretion udmna hsc ihLISA with physics Fundamental WNotes GW

83 oe esfrG science GW for News & Notes Notes & News for GW science 84 WNotes GW ai lxVraiiyo g A* Sgr of Variability Flux Rapid (and models current to AGN. led and has BHB this both in how flow spectral and accretion XSPEC the use 1996), available of to al controversies) publicly how et the bina- discuss (Arnaud using hole also package data black I fitting real of (AGN). interpret variability Nuclei physically and these Galactic to spectra how Active these the on and interpret focus BHB) to I (hereafter here toolkit textbook, ries a any as in used found be be can can processes basic the While Eprint: Authors: apparent singularity ring and horizons hole black multi of Study thick optically of ex- regions to energetic close of speeds explosive, at expansion of events presence the pansion the through suggests fluctuations arise this scale mm plasma, time 7 synchrotron-emitting minute emit- at the the that emission of Assuming size the AU. 0.1 the of than constrains less variability be scale to These time region to ting short sub-minute This and wavelengths. from variability hours, scales. radio continuous several time at for hourly to case variability seconds strong scale few a a time suggest from measurements sub-minute ranging for scales evidence time on find A* Sgr of ability of durations Abstract: Keywords: Eprint: N. Grosso, Authors: g *ta edtebs fa uflwo jet. of or outflow flow an accretion of the base in the fluctuations feed vari- from that quiescent result A* or could Sgr emission but variable understood scale not time is short en- ability such an short of on as detected nature mainly are The interpreted that scales. flares then time overlapping is and A* weak Sgr numerous from of average component emission semble steady 1.3mm at This observed A*. scale Sgr 0.1AU resolved of compara- spatially is averaged time time travel the light to one-minute ble to corresponding length scale inferred be The to estimated are component this of loss http://arxiv.org/abs/1008.2001 http://arxiv.org/abs/1008.2229 aail,Gbil;Lut,Cro O. Carlos Lousto, Gabriela; Jaramillo, g *ehbt ae nrdo ilmtradsbmwvlntswith wavelengths submm and millimeter radio, in flares exhibits A* Sgr ue-ae,F;Wrl,M;Mle-oe,J;Rbrs . oqe,D.; Porquet, D.; Roberts, J.; Miller-Jones, M.; Wardle, F.; Yusef-Zadeh, sr-hG;atohsc;osrain;SgtaisA* Sagittarius observations; astrophysics; astro-ph.GA; ∼ 1 or sn tutr ucinaayi,w netgt h vari- the investigate we analysis, function structure a Using hour. udmna hsc ihLISA with physics Fundamental c h eurdrt fms rcsigadenergy and processing mass of rate required The . & 6 × 10 etme ,2010 7, September − 10 M

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respectively. oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 oooy efudta odetmt o hsrn rtclrdu is radius toroidal critical of ring horizon this for event estimate an good generate a would that that found radius We The effort ring an topology. in radii. critical horizon different event a horizon the of of predict apparent singularity location the to the ring of study indicative a as then of used We is geometry horizon apparent initial case. symmetric hole time black the for binary of cases mass mass unequal equal the aligned to the detail in study We of systems in horizon apparent Abstract: relativity numerical holes; Keywords: hog h othl n a edtcal ssailyofe cienuclei. active spatially-offset as detectable be wander will may km/s and 300-600 halo range host the gas the in of speeds through effect recoil recoil the with of remnants MBHs mergers case and weaker, minor the is in be in drag 4) can remnants km/s; merger nuclei 700-1000 major range offset in the kinematically in Myr 3) velocities few center; a of host’s timescales the for km/s from observed 1200 kpc of 1 velocities kick within with remain MBHs to even mergers, allows major gas remnants, in high-density merger 2) from minor case; drag this the in in significant signatures more electromagnetic is for allowing contribution potentially This thermody- gas. in the rotation- the 1) to the of contribution into namics that: negligible a hole show makes moving We medium the turbulent by systems. supported, semi-analytical ally deposited gas-rich a energy in the construct MBHs remnants to of merger data major evolution numbers new simulation orbital Mach run use the We with and for remnant successful. km/s, model merger be 1

85 oe esfrG science GW for News & Notes Notes & News for GW science 86 WNotes GW Eprint: G.; Trap, D.; Porquet, A.; Goldwurm, G.; Bower, O.; F. Pfuhl, Yusef-Zadeh, H.; Bartko, T.; Ott, R.; zel, Authors: bright variabil- near-infrared: continuous the low-level of ity in top A* on Sgr flares episodic of states two The Keywords: Eprint: Authors: Formation Structure Sce- of Hierarchical nario in Systems Binary Hole Black Massive A*. brighter Sgr 40% from and observed Ks-band, ever the in flare S2 brightest star next the the of than brightness the double to close A*, Sgr flux Ks-band intrinsic ( an Ks-band mJy reached brightest the 27.5 which the of 2008) of here 5th, and report August also emission (from We observed flaring state. ever as flare quiescent mJy the 5 as emission above level emission low general level a low make We expected the fluxes. than of high to common) identification distribution more lognormal the are of events extrapolation the flux for (high flatter significantly is of tribution flux with distrib- median dereddened mJy, lognormal a 5 a has about distribution by than lognormal described (less be fluxes can intrinsic low distribution timescales at flux on ution The variability medium-term months. near- some to the be weeks in to of varying) two appears is and also with A* ‘on’ there A* Sgr always and find is Sgr infrared, We source of the distribution. variability (meaning flux variable the its continuously investigate analyze We and methods ob- photometric NACO/VLT 2009. different from to set 2004 data Ks-band taken extensive servations very a using (NIR) near-infrared Abstract: holes black Keywords: http://arxiv.org/abs/1008.0399 http://arxiv.org/abs/1008.1984 eer,EuroS;Mrna sad D. Oswaldo Miranda, S.; Eduardo Pereira, od-dn . ilse,S;Fiz .K;Esnae,F;Tip,S;Gen- S.; Trippe, F.; Eisenhauer, K.; T. Fritz, S.; Gillessen, K.; Dodds-Eden, nti ae eeaiepoete ftevral oreSrA nthe in A* Sgr source variable the of properties examine we paper this In sr-hC;csooy ik/eol asv iaiso lc holes black of binaries massive kicks/recoil; cosmology; astro-ph.CO; sr-hG;atohsc;osrain;SgtaisA;supermassive A*; Sagittarius observations; astrophysics; astro-ph.GA; m Ks = 13 . 5 .Ti aewsafco 7ices vrtemda u of flux median the over increase 27 factor a was flare This ). udmna hsc ihLISA with physics Fundamental ∼ . J,btaoe5myteflxdis- flux the mJy 5 above but mJy, 1.6 etme ,2010 7, September A Ks =

2 .

5 .The ). oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 on (say, point obns3Nkoldeat knowledge 3PN combines O aaees otsgicnl,w bev htan that observe we tation significantly, Most parameters. EOB of terms PN higher-order to access ρ give orders. data PN GSF higher that at demonstrate occurring ana- we terms the Furthermore, logarithmic-running account the into of taking some when of the improved values is lytic in agreement well this that agree and results results, con- our EOB the that (small of show We regime description (EOB) weak-field systems. Body binary One of Effective dynamics the servative entering functions basic the the time, first function the the for of mean determines, computation the GSF with Our associated orbit. radius) circular over (mass potential gravitational dimensionless h ri,adwhere and orbit, the determine to way a describe MBH. of we systems Also, binary rate of holes. merger number the black the for massive form contains analytical that the account haloes for- into Press-Schechter of take the the to Laser use extention that we the its expected work, and by is malism this detectable In It signal (LISA). waves Antenna systems. gravitational Space a binary Interferometer produces MBH MBH of mergers two formation that of suppose the merger can to we are context, leads clusters this galaxies galaxy In of and objects. scenario small galaxies hierarchical of like mergers the objects by hand, formatted which other describe the formation On structure (MBH). of holes black massive are there Abstract: esratio less mass of mass particle of a function hole gauge-invariant of black orbits Schwarzschild small-eccentricity a the around ing of rate precession the the compute to we (GSF), self-force gravitational gauge Abstract: Keywords: Eprint: Authors: a in self-force malism for- gravitational one-body effective the the and spacetime Schwarzschild of effect Precession ( x ) n a eue ostueu e osrit ntevle fyet-undetermined of values the on constraints new useful set to used be can and of http://arxiv.org/abs/1008.0935 ρ ( aak er aor hbut ao Norichika Sago, Thibault; Damour, Leor; Barack, eety thsicesdteosrainleiec ht nms galaxies most in that, evidence observational the increased has it Recently, Ω sn eetypeetdnmrclcd o acltn h Lorenz- the calculating for code numerical presented recently a Using ( x ˆ x fetv n oy MI rq;ps-etna hoy spin theory; post-Newtonian gr-qc; EMRI; body; one Effective r = ) / Ω a eotie sn ipetopitPd prxmn which approximant Pade two-point simple a using obtained be can ˆ 1 / ϕ 6 ) 2 ). ewe h qae fterda n zmta rqece of frequencies azimuthal and radial the of squares the between x = ρ udmna hsc ihLISA with physics Fundamental [ x ( Gc x ihte3dps-etna P)epnino the of expansion (PN) post-Newtonian 3rd the with ) ) where , − x 3 ( M = togfil behavior strong-field 0 + ihGFifraina igestrong-field single a at information GSF with ρ m sdfie sthe as defined is ) WNotes GW Ω ˆ ϕ ] 2 / 3 sagueivratmaueo the of measure gauge-invariant a is M  ρ ( O m x O ) ( pcfial,w td the study we Specifically, . facmiaino w of two of combination a of m nteinterval the in ( xeln lblrepresen- global excellent m ) ) osraiecorrection conservative ato h dimension- the of part 0 < m x ≤ mov- 1 / 6

87 oe esfrG science GW for News & Notes Notes & News for GW science 88 WNotes GW h asi,adters rssfo raices ertecutc nue ythe by induced caustic, the near through object. increase horizon compact area the the from of enter arises field gravitational rest that the generators and from leading-order caustic, arises the the among half that show increase, further is We area It plunge. horizon inde- the horizon. is of that the details geometry the into the of of plunges pendent characterization particle is analytic the an it obtain which to that at as- possible therefore show simple point we have the exist turn near caustic, to in forms the shown which propa-ymptotic near perturbations, is by geometry large-l caustic by the horizon A predominantly on event determined Focusing new horizon. merger. the unperturbed the find the before then near geodesics object, use null in- compact perturbations first gating small We metric this the hole. calculate by to black duced formalisms Schwarzschild Zerilli large and a Regge-Wheeler into the plunges object compact small Abstract: Keywords: Eprint: Mass-Ratio Authors: Extreme Mergers in Hole Black Deformations Horizon Event hs otNwoinefcs eetmt h pcrlrslto eurdt detect to of required detection resolution spectral the the for estimate allow We will effects. post-Newtonian resolution these sufficient of measurements Spectral shift. and order space, at curve terms enter Schwarzschild leading-order The of velocities. Saha inclusion line-of-sight The & the 2010). order Kannan Saha at 2006, & dilation (Angelil al., time Minkowski gravitational et the post-Newtonian from (Zucker The photons Keplerian the the and channels. 2009), from distinct orbit two the via perturbs dynamics perturbations regime the GR-induced The enter light. redshift of the speed the to of percent few a of velocities reach Abstract: Keywords: Eprint: Authors: Stars Galactic-centre with GR Testing http://arxiv.org/abs/1008.1061 http://arxiv.org/abs/1007.5387 ael,Ra;Ce,Yanbei Chen, Ryan; Hamerly, nei,Ryod aa Prasenjit Saha, Raymond; Angelil, h aatcCnr -tr riigtecnrlsprasv lc hole black supermassive central the orbiting S-stars Centre Galactic The esuytegoer fteeethrzno pctm nwiha which in spacetime a of horizon event the of geometry the study We sr-hG;atohsc;ER;g-c aitru * tla dynamics stellar A*; Sagittarius gr-qc; EMRI; astrophysics; astro-ph.GA; MI eea eaiiy gr-qc relativity; general EMRI; v 3 h lsia elra hnmnlg oiae h oa red- total the dominates phenomenology Keplerian classical The . udmna hsc ihLISA with physics Fundamental v 2 ak h rtdprueo h esitfrom redshift the of departure first the marks

etme ,2010 7, September oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 pcrldt fS ihadseso faot1k/ ol lo o la de- leading-order clear for a suffice for would allow km/s would detection. 1 curvature 10km/s about that space about and argue of redshift, We gravitational dispersion of a terms. tection a with relativistic S2 with the of one effects, between relativistic data - the distinctions spectral orbit amplifies visual This S2 S2. clear exaggerated real allows an the of with and that play of We fraction plus a elements data. axis keplerian semi-major mock five to the via mass curve hole redshift the black fitting by effects these of each eaiitcmgeoyrdnmcl(DGMD iuain o dimensionless general for three-dimensional simulations spins run GRMHD) We (3D set. magnetohydrodynamical quasi-quiescent from relativistic a observations into The averaged observations. are sub-mm polarized papers fitting by found are ters Abstract: Keywords: Eprint: Authors: Model- General ing Radiative by Polarized A* and Sgr Dynamical in Relativistic Flow Accretion the Constraining spin is spin angle probable most position the a vector reveals electric analysis and statistical (CP), Our (EVPA). polarization circular (LP), polarization ear ossetwt h bevdb LItechnique. VLBI by observed the with consistent at sizes region sion T gives M efr Rplrzdrdaietase,adepoeteprmtrsaeo spin T of space parameter the angle explore inclination and transfer, radiative polarized GR perform otgtycntansm uniis nlnto nl,eeto eprtr,and temperature, electron angle, ranges Inclination have angle quantities. position some constrain tightly to a with ˙ e e = = at = = 0 0 1 . a 6 3 90% . 9 5 χ . a M . 3 50 = eget we 2 ouin are solutions http://arxiv.org/abs/1007.4832 · = ais h etfitn oe o spin for model best-fitting The radius. 10 = 0 hhrao,RmnV;Pna oetF;MKne,Jnta C. Jonathan McKinney, F.; Robert Penna, V.; Roman Shcherbakov, · ofiec.Tettlrneo crto aei ag,btasmn spin assuming but large, is rate accretion of range total The confidence. h osrit nSrA lc oe(H n crto o parame- flow accretion and (BH) hole black A* Sgr on constraints The 0 10 − secue shvn probability having as excluded is 0 , sr-hH;atohsc;osrain;SgtaisA;spin A*; Sagittarius observations; astrophysics; astro-ph.HE; 8 . 0 10 84 M . M 5 ˙

.W dniytepyia hnmn edn otemthdlin- matched the to leading phenomena physical the identify We K. , with (0 0 year θ . . 7 9) oiinage(A,aceinrate accretion (PA), angle position , , 230 0 − = 10 . θ 1 9 , , 13 = T 0 ie espoal ept iiglwrminimum lower giving despite probable less times H ftebs-tigmdl r on ob marginally be to found are models best-fitting the of GHz . e udmna hsc ihLISA with physics Fundamental − + 98 70 3 4 = × θ ◦ till 3 10 , . = 2 M − ˙ · 20000 59 9 10 M = ◦ 10

7 ± year . at K 0 M 9 · WNotes GW ◦ osrc naeae yaia model, dynamical averaged an construct , , 10 − T 6 1 − M e nevlwith interval 8 = M h etfitn oe o spin for model best-fitting the , P

3 ( a a year . 4 ) = − + < 0 1 0 . . 9 2 . − 9 1% 1 × M and , gives ˙ 10 oaie aaalw us allows data Polarized . n lcrntemperature electron and , 90% 10 T K χ ofiec.Teemis- The confidence. p 2 and , / = T e 0 a = . 99 = PA 22 0 with . = 9 at h spin The . 96 6 θ M ◦ χ a = 2 ± = with and 59 30 0 29 . a ◦ 5 ◦ , ,

89 oe esfrG science GW for News & Notes Notes & News for GW science 90 WNotes GW B?()Wa steoii fteselrds(),ad()Wa steoii fthe of origin the is What (4) and the disk(s)?, around stellar cusp" the "dark of a origin S-stars? there the Is (1) is (2) are What relaxed? questions (3) MBH The MBH? the them. around addressing galactic system in stellar and made the MBH progress Is Galactic the the and of general, in environment nuclei the both understanding for cations Abstract: dynamics stellar A*; Sagittarius Keywords: Eprint: Authors: dynamics Center Galactic about questions Key Eprint: Authors: Likelihoods Lazy and Matrices Fisher Fast available other to the respect while with account, emis- models. reduced into significantly disc taken is the easily data precomputed be of of can amount dependence laws darkening radius limb Based arbitrary arbitrary an programs. and sivity analysis approach, data function mod- X-ray Green’s for in code a a scheme on present stable this and with discs be such data to for observational shapes assumed elling line are discuss We configurations 2005). the al., both to et includes as respect (King with scheme momentum, antiparallel The angular and hole’s parallel holes. are black which black momenta rotating angular around with discs discs accretion from lines sion Abstract: holes black supermassive parts; Keywords: Eprint: black spinning Authors: negatively for holes lines emission Broad http://arxiv.org/abs/1007.4820 http://arxiv.org/abs/1007.4937 http://arxiv.org/abs/1007.4991 lxne,Tal Alexander, ons,Ni J. Neil Cornish, W. L. Brenneman, S.; C. Reynolds, J.; Wilms, T.; Dauser, epeeta xeddshm o h aclto ftepolso emis- of profiles the of calculation the for scheme extended an present We ics orkyqetosaotGlci etrdnmc,terimpli- their dynamics, Center Galactic about questions key four discuss I sr-hG;atohsc;ER;IR;itreit-asbakholes; black intermediate-mass IMRI; EMRI; astrophysics; astro-ph.GA; crto ic;atop.O sr-hH;atohsc;E counter- EM astrophysics; astro-ph.HE; astro-ph.CO; discs; accretion udmna hsc ihLISA with physics Fundamental

etme ,2010 7, September oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 a eue osedu aeinifrneapidt elgaiainlwv data. wave gravitational real to techniques applied related inference Bayesian how up describe speed to I waveforms, used be full savings. can compute de- computational to I significant need Here the in sidesteps resulting waveforms. that gravitational technique computing alternative an of direct scribe a step in costly which the functions, entail Likelihood approach and Matrices Information Fisher of culation Abstract: forms Keywords: ml lc oemse agn rm30to 3.0 from Centauri ranging omega for masses models hole dynamical a Isotropic black provides hole. which imply black km/s, central 22.8+-1.2 the a to in for region rise sign a central strong see the We a in set. show dispersion data motion velocity and proper radial view large a of from field results the smaller data with a The discrepancy for literature. performed the from measurements centers previous different existing support de- two with new and a data kinematics account from these into center combine taking rived We profile dispersion velocity Centauri. radial omega the of of spec- measurements integrated region new central obtain contradic- the to VLT-FLAMES to for use lead tra We measurements issue. Recent this on hole. conclusions tory black mass intermediate an hosting Abstract: vations Keywords: Eprint: Holger Baumgardt, Tim; P. Zeeuw, de Behrang; Jalali, Authors: Support Hole Further Black Central a Centauri: for omega for Kinematics VLT Eprint: Bernd mann, Authors: spins non-precessing with binaries Black-hole h etr h etfitdms is mass best-fitted The center. the http://arxiv.org/abs/1007.4559 http://arxiv.org/abs/1007.4789 hoeia tde ngaiainlwv srnm fe eur h cal- the require often astronomy wave gravitational in studies Theoretical ooa v;Gbad,Kr;KslrPtg aks uzedr,Nora; Lutzgendorf, Markus; Kissler-Patig, Karl; Gebhardt, Eva; Noyola, anm ak ua aca he rn;Melr oen Brueg- Doreen; Mueller, Frank; Ohme, Sascha; Husa, Mark; Hannam, h aatcgoua lse mg etuii rm addt for candidate prime a is Centauri omega cluster globular Galactic The sr-hG;atohsc;IR;itreit-asbakhls obser- holes; black intermediate-mass IMRI; astrophysics; astro-ph.GA; aaaayi;g-c aaee siain erhagrtm;wave- algorithms; search estimation; parameter gr-qc; analysis; data udmna hsc ihLISA with physics Fundamental 4 . 7 + − WNotes GW 1 . 0 × 10 5 . 2 4 × oa masses. solar 10 4 oa assdpnigon depending masses solar

91 oe esfrG science GW for News & Notes Notes & News for GW science 92 WNotes GW Keywords: in nti ae,w hwta,i h nlsaeo h ytmi lc oe then hole, black a is system the of O state final to the correction if leading that, the show we paper, this In to tion. corrections radius finite of understanding An and to radius. extraction carried finite energy some at of flux the and times, source, the from observers, far distant waves particular gravitational of scalar of Weyl Quantities flux the are spacetime. calculations many dynamical for strong-field interest a by generated waves Abstract: Keywords: Eprint: space- hole Authors: black in energy radiated times of falloff the On is BH each of parameter q before spin orbits the ten branch, and spinning χ six equal-mass between the complete Along that merger. Einstein’s binaries of black-hole solutions unequal- numerical for nonspinning from equations calculated and are waveforms spins, The space: non-precessing binaries. parameter mass equal BBH with the of binaries branches equal-mass two along systems (BBH) black-hole-binary Abstract: forms ti osbet ra alr4i uhawyta tgvstebs cuayfrspins for accuracy best the gives the it of that way but a performance, such robust in χ most TaylorT4 (in- treat the to gives approximant possible order) TaylorT1 is 2.5PN it 3.5PN only to the up nonspinning binaries terms for spin spinning accurate cluding equal-mass most is For approximant TaylorT4 that binaries. find 3.5PN the we the compare studies, from and previous phase in BH, the As merged approximants. final (PN) to the post-Newtonian up standard of cycles properties GW the 8-10 cases, last these for data tial i i (1 = > = / M E r − ˙ 2 S 0 ( ) losu omr cuaeyifrteraypoi ausfo computa- a from values asymptotic their infer accurately more to us allows 2 ψ i ` . / / http://arxiv.org/abs/1007.4596 and 75 4 M M = uk,Lo . uhs ct A. Scott Hughes, M.; Lior Burko, ∝ hnhg-re mltd orcin r nldd h Namplitude PN the included, are corrections amplitude high-order When . i 2 1 h olo uhrsac nrltvt st nesadgravitational understand to is relativity in research much of goal The epeetgaiainlwvfrsfrtels risadmre of merger and orbits last the for waveforms gravitational present We 2 eea eaiiy gr-qc relativity; general rq;msiebnre fbakhls ueia eaiiy pn wave- spin; relativity; numerical holes; black of binaries massive gr-qc; , 1 O ∈ ∈ m / (1 r [1 [ = − / and , r 0 ± 4] 3 E . ˙ ) 2) 85 edsustecntuto flwecnrct ucueini- puncture low-eccentricity of construction the discuss We . osrainlw urne ht nayptclyfltspace- flat asympotically in that, guarantee laws Conservation . soemgtnieyges u ruetol eiso the on relies only argument Our guess. naively might one as E , ˙ oe slre hnteN mltd ybten2-4%. between by amplitude NR the than larger is modes 0 ∝ . 85] ψ udmna hsc ihLISA with physics Fundamental 1 / 4 n ln h nqa-asbac h asrtois ratio mass the branch unequal-mass the along and , M r is 2 ω as O = (1 r / ∞ → 0 r . 3 1 ) n htt h nryflxis flux energy the to that and , ihtepaeadapiuepeitdby predicted amplitude and phase the with otcluain xrc hs quantities these extract calculations Most . etme ,2010 7, September ψ 4 hc ssml eae othe to related simply is which , O (1 / r 4 ) not —

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4 oe esfrG science GW for News & Notes Notes & News for GW science 4Spebr7 2010 7, September #4 sqiees ocretfrfiieetato aiseffects. it radius that extraction showing finite per- for falloff, hole correct leading to black the easy Using to quite corrections is spacetimes. the hole calculate black we theory, for turbation scalars curvature the of behavior Abstract: Keywords: Eprint: Authors: Supply Gas Formation Star Nuclei: by Driven Galactic Active in Disks Accretion Abstract: Keywords: Eprint: Authors: Supermas- Holes High-Redshift Black of sive Detection and Origin The optn cnro.Ias reymninsm oeeoi da n o the how instruments. other and and ideas LISA two by exotic these future more the review in some I distinguished mention be contribution, may briefly this models different also In where I environments stars. special rare into scenarios. metal- in fragmenting competing of gas avoid generation of can collapse first direct gas the rapid the by the behind by left growth or BHs Eddington-limited stars, free seed of stellar-mass combination z=6. of redshift the at mergers by exist and arise already may masses SMBHs solar earliest billion several These as massive as SMBHs and nAN.A eiso Frgos ig(rbl)cnitn fodsasrmisfor stellar remains multiple stars that old suggest of We consisting activity. belt) hole (or black ring supermassive a of regions, episode SF every of observed relics present that As The with spontaneously. AGNs. consistent produced in relationship are dri- metallicity–luminosity metals be a and can predicts AGNs regions model in the rates in typical SNexp with disks by to accretion ven acting that regions find (SNexp), We the in explosion scale. momentum 1pc supernovae angular within of of transportation role the the in viscosity, explore turbulent We full excite dynam- A the regions. describe (AGNs). to the nuclei given of is galactic formation ics active star in of feedback torus including dusty equations the of set of edge inner the to tending http://arxiv.org/abs/1007.4741 http://arxiv.org/abs/1007.4060 ag .-. a,C S;Go .-. u . i .-. hn,S. Zhang, -R.; Y. Li, C.; Hu, -Q.; H. Gao, -S.; C. Yan, -M.; J. Wang, Zoltán Haiman, uemsiebakhls(MH)aecmo nlclglci nuclei, galactic local in common are (SMBHs) holes black Supermassive efgaiaigaceindssclas osa-omn(F ein ex- regions star-forming(SF) to collapse disks accretion Self-gravitating crto ic;atop.O srpyis Mcounterparts EM astrophysics; astro-ph.CO; discs; accretion holes black supermassive cosmology; astro-ph.CO; udmna hsc ihLISA with physics Fundamental WNotes GW

93 oe esfrG science GW for News & Notes Notes & News for GW science 94 WNotes GW urn n uuerdainbc-ecinmdl o erplrrtord orbits. retrograde near-polar for models back-reaction radiation future of and current evolution the studying for laboratory neon ence utfrtewa edrdainrato,w on h pe ii on limit upper the of found range we full radiation-reaction, field weak the for sult Eprint: Mas- Authors: orbits circular a I. About Hole: Orbits Black Kerr Inclined sive for Constant Carter The episodes after cluster star formation. nuclear star a by form driven and interact directions random with rings n cetiiy( eccentricity retro- and and prograde the which between at Schwarzschild abutment orbits a the grade represent For orbits polar models. the reaction hole, black radiation complements and of independent ( constant Carter the of iour ( inclination Abstract: Keywords: efidta h eodadhge eiaie of derivatives higher and second the that find we aigtelmto hseuto for equation this of limit the taking h btet oa ris n atsal ris(S) ykoigteanalytical the knowing By (LSO). orbits stable of last form and orbits, polar abutment, work the this of evolution extended for the then formulae of and analytical understanding the better KBH, oped a investigated a develop first To about we test-particle orbits. general a (KBH), to of hole (LSO) black orbit Kerr stable a last of abutment the characterise To orbits. retrograde and prograde separates inclination; cleanly orbital greater longer towards no moved it be thus to abutment, or boundary, this causes loue hs omlet ueial aclt the calculate numerically to formulae these used also rista vleaogteaumn.Fo hs ausw aedtrie that determined have we values these From ∂ι/∂ abutment. the along evolve that orbits l ˜ = http://arxiv.org/abs/1007.4189 − ∂ ∂ι/∂ Q ooosi .G;Vlui .R;Hue M. Houde, R.; S. Valluri, G.; P. Komorowski,  na xrm iaybakhl ytm nobtwl nraeisageof angle its increase will orbit an system, hole black binary extreme an In 122 /∂ MI eea eaiiy edscmto;gr-qc motion; geodesic relativity; general EMRI; ι l l ˜ ˜ si vle nKr pctm.W ou u teto ntebehav- the on attention our focus We spacetime. Kerr in evolves it as ) hsteaumn eoe niprataayia n numerical and analytical important an becomes abutment the Thus . l ˜ pt h S.Atog eko h au of value the know we Although LSO. the to up . 7 tteaumn,w eeal ots P u qainfrQ We Q. for equation flux 2PN a test to able were we abutment, the at S ˜ e − .Teitouto fsi ( spin of introduction The ). 36 S Q ˜ 3  sa t aiu au o ie auso au etm( rectum latus of values given for value maximum its at is l ˜ udmna hsc ihLISA with physics Fundamental − 11 Q / 2 Q o erplrobt;addvlpa nlssta is that analysis an develop and orbits; near-polar for ) − ntrsof terms in  63 l ˜ / 2 ∞ → S ˜ + Q n oprn twt h ulse re- published the with it comparing and , 35 l ˜ and , / e 4 and , S ˜ S ˜ etme ,2010 7, September ι 3 =  nKr pctm n o testing for and spacetime Kerr in Q l ˜ | − J | S 9 ihrsetto respect with ˜ / / M 2 odsrb litclobt at orbits elliptical describe to ∂ι/∂ − 2 otemsiebakhole black massive the to ) 15 l ˜ / fhpteia circular hypothetical of 2 ∂ Q S ˜ l ˜ /∂ − 7 / l ˜ 2 tteabutment, the at l − ˜ xr ninflu- an exert 9

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95 oe esfrG science GW for News & Notes Notes & News for GW science 96 WNotes GW C2.5 a pcrmrdoqaa tz048 bevdi h DSadi a Hbeta (FWHM in The profiles and broad Telescope. SDSS show Optical the lines Nordic in Halpha the and observed from z=0.4183 follow-up at spectroscopic quasar dedicated radio spectrum flat a 4C+22.25, Abstract: Keywords: Eprint: eaindfie yelpia aais eso,nwwt eypeieB mass BH the precise below very fall with between relation group now power-law show, a low-scatter We as the that galaxies galaxies. measurements, maser of elliptical five The by of defined subset imaging. at relation a SDSS telescope of m with decomposition 3.5 galaxies bulge-to-disk the perform these on spectro- also spectrograph We B&C DIS the the Point. and Apache using telescope observations Dupont exquisite the long-slit with on on masses graph nine the based of BH of sample galaxies yields Modeling a disk for BH. (2010), measurements megamaser central dispersion the velocity al. from stellar et present pc We Kuo a precision. of by tenths presented few molecular curves, a circumnuclear rotation of of radii rotation at Keplerian starting the disks trace using masers mass, The H in of disks. lower dynamics magnitude nuclear the of from order derived an measurements are mass that BH BHs probe rep- to typical not limitations more do prior however, of objects, demographics These the kinematics. resent maser and ( is gas, stellar, masses correlations direct these BH using of of high decade knowledge to Current last predominantly the limited evolution. influenced galaxy greatly understand have to correlations effort (BH)-bulge hole black The Abstract: Keywords: J. M. Eprint: Reid, C.; Henkel, Y.; K. Lo, J.; J. Condon, V.; M. Disks: Megamaser Authors: Mass From Low at Relations Masses Hole-Bulge Black Hole Black Precise of limitations and two virtues of the discuss superposition scenario. we binary the and hole on black holes, of massive based black lag a interpretations recoiling time on possible a or out in emission sources variation rule narrow We significant the no to show frame). respect features These with km/s) lines. v=8,700+/-1,300 (Delta offsets treme http://arxiv.org/abs/1007.2851 http://arxiv.org/abs/1007.3738 ree .E;Pn,C . i,M;Ko .Y;Bat,J . melzei C. Impellizzeri, A.; J. Braatz, Y.; C. Kuo, M.; Kim, Y.; C. Peng, E.; J. Greene, erpr h icvr fpcla etrsi h pia pcrmof spectrum optical the in features peculiar of discovery the report We sr-hC;atohsc;msiebnre fbakhls observations holes; black of binaries massive astrophysics; astro-ph.CO; sr-hC;atohsc;osrain;sprasv lc holes black supermassive observations; astrophysics; astro-ph.CO; udmna hsc ihLISA with physics Fundamental L M < BH ∼ L etme ,2010 7, September ∗ 200k/) an ue n ex- and fluxes faint km/s), 12,000 & aais hssuytranscends study This galaxies. 10 8 M 2 eaaesi circum- in megamasers O

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97 oe esfrG science GW for News & Notes Notes & News for GW science 98 WNotes GW rqec,pr rvttoa aei ctee rmabakhl,asaa aeof wave scalar a vice-versa. hole, and black excited, a high is from a amplitude scattered when comparable event that is the reveals wave further of gravitational analysis location pure The frequency, un- the unaltered. is is waves propagation spacetime gravitational the Radial by of horizon hole. probed black as the the that with from implying propagation decreases distance and affected, the the hole, of black of the power components of inverse mass azimuthal third the the to proportional on linearly The depends is superluminal. vector, splitting one and the subluminal of one How- modes, width along two spacetime. propagation into Minkowski splits of direction speed in given characteristic light a the of background speed Schwarzschild the a waves at on ever, gravitational travel that theory stable reveals modified linearly also the is analysis it in Our that considered. find backgrounds and approximation the optics on geometric the in gravity fied Abstract: Keywords: a atr h olna set fha-nbnr-lc-oemresaccessible collision. mergers the binary-black-hole from head-on far observers of to solutions aspects black-hole nonlinear exact merg- the to perturbations head-on capture linear for can that radiation imply further gravitational suffice would outgoing may This of theories ers. features BHP main and the PN that explain suggest to results radiated the Our and momentum. waveforms and gravitational energy the simulation, between numerical-relativity agreement We good full find ap- spins. a we anti-parallel we and with transverse, and technique with holes theories, approximation black BHP our of and compare collision PN head-on introduce the of we to elements paper, it incorporates ply this that In method merger. hybrid the non- a characterize the and spacetime ringdown, of the dynamics describes linear theory inspiral (BHP) the treats perturbation approximation black-hole (PN) phase, post-Newtonian The ringdown. and merger Abstract: Keywords: Eprint: Authors: case head-on mergers: black-hole understanding for method hybrid A http://arxiv.org/abs/1007.2024 ihl,DvdA;Ce,Yanbei Chen, A.; David Nichols, lc-oebnr olsec sotndvddit he tgs inspiral, stages: three into divided often is coalescence Black-hole-binary epromalna tblt nlsso yaia hr-iosmodi- Chern-Simons dynamical of analysis stability linear a perform We sr-hC;atop.A rq;hpt;tsso lentv theories alternative of tests hep-th; gr-qc; astro-ph.GA; astro-ph.CO; rq;ps-etna hoy waveforms theory; post-Newtonian gr-qc; udmna hsc ihLISA with physics Fundamental

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etme ,2010 7, September oe esfrG science GW for News & Notes

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