October 2009 to March 2010 Notes & News for GW Science

GW Notes

October 2009 to March 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 involved 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 advancement that they draw closer, and that they speak a common idiom. Notes & News for GW science 3My2,2010 21, May #3 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

1 oe esfrG science GW for News & Notes Notes & News for GW science 2 WNotes GW 1 a mr-eae&BradF cuz editors Schutz, F. Bernard & Amaro-Seoane Pau article. highlight our for holes black massive around aso h ev lgt opnnsand components a (light) heavy which when the in of situation mass i.e. the occurs, to segregation the study mass revisited the “strong” (2010) extended gravita- Amaro-Seoane and low-frequency problem and to Bahcall-Wolf Preto also classical Recently, but dynamics, Astrophysics. stellar wave to relevant tional which only obvious the problem not to a due has authors, is it many hole by applications times, black of massive number a a addressed around been has stars distributes gravity way The rt mr-eae21a 00 n mr-eae rt ria 2010 Freitag & Preto Amaro-Seoane, and 2010b 2010a, Amaro-Seoane & Preto o hsG oe su ehv se iulPeo(edlegUiest)to University) results (Heidelberg new Preto some advance Miguel to asked and have work recent we this issue expand Notes GW this For intermediate- and extreme- both be to events. steeper candidates inspiral a of ratio since number mass straightforward, higher are a waves to gravity leads stud- of previous cusp terms also in and implications observations The both with ies. agreement in is which cusp, steeper M where solution, Bahcall-Wolf the veriﬁed M they program, direct-summation a using odcigadtie td fdfeetsseswt different with systems different of study detailed a Conducting h h r omnadtu oiaetebhvo ftesse.I h aei which in case the In system. the of behavior the dominate thus and common are r ae ev tr ikt h etrb yaia rcinadbidteea there build and friction dynamical by center the to sink stars heavy rare, are o tr itiueaon asv lc hole black massive a around distribute stars How tla up nglci nuclei galactic in cusps Stellar Editorial N h ( N n h l a 1 2010 21, May hi oa nta number. initial total their ) M h 2 < n l m 1 nhwsasdistribute stars how on l 2 where , M h , N h M , m h l ( m and l sthe is )

l by oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 -al [email protected] e-mail: Germany Heidelberg, 12-14 Mönchhofstr. (ZAH) Institut Rechen Astronomisches Preto Miguel HOLE BLACK MASSIVE A AROUND DISTRIBUTIONS STELLAR I. CLUSTERS STELLAR NUCLEAR OF EVOLUTION DYNAMICAL ino the of tion N asdtcal yLS ilb oiae yteisia fselrms lc holes. black stellar-mass of inspiral the inspi- by ratio dominated mass be extreme will of LISA rates by the to detectable consequence, rals close natural regions a As innermost the hole. black in massive density the spatial of the regime dominate the holes black in stellar-mass is cluster the functions, mass mass of hole black massive central in clusters a stellar with nuclear state for steady conﬁguration natural the are cusps stellar segregated Mass bd n okrPac tde ge ut elwt ahohri h descrip- the in other each with well quite agree studies Fokker-Planck and -body bulk o tr itiueaon asv lc hole black massive a around distribute stars How rpriso h tla itiuino uhsses o yia initial typical For systems. such of distribution stellar the of properties WNtshglgtarticle highlight Notes GW tla cusps Stellar Abstract WNotes GW strong M assgeainadtherefore and segregation mass • . few × 10 6 M

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3 oe esfrG science GW for News & Notes Notes & News for GW science 4 WNotes GW 3 2.4 2.3 2.2 2.1 2 1 Contents umr n icsin21 5 7 discussion and Summary MBH a around NSCs of distribution Stellar Introduction -oyvldto 16 11 13 7 validation N-body Cusps Segregated Mass Cusp Wolf & Bahcall models and quantities Basic o tr itiueaon asv lc hole black massive a around distribute stars How

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5 oe esfrG science GW for News & Notes Notes & News for GW science 6 WNotes GW Glesne l,20) h eietrdsac fsm fteesasi inferred is stars these of some of distance pericenter The be to 2009). al., et (Gillessen n tr nhgl ceti,nal elra risaon B of MBH a around orbits Keplerian mov- fast nearly of eccentric, population highly a are in center individual stars Galactic of future—the ing the measurements in foreseable detailed stars innermost have the The to in orbits. hope stellar remain may one will which is—and for nucleus Galactic-center only the in NSC Preto The and 2009 the Hopman, towards and heavier the Alexander 2010a). Amaro-Seoane, of 2006b, the and accumulation Alexander, impact the and strongly favors (Hopman also it center function—will since mass rates, stellar dynami- EMRI realistic natural expected any the is for segregation—which outcome Mass cal originate to 2005). expected Alexander, are sources and inspiralling (Hopman these which from distance the is which a lc oe SH) nodrt ietnl ohefcsfo bevtoswill perturbations observations Galactic 2009). from and Saha, effects effects and both (Preto post-Newtonian disentangle for stel- simultaneously to and ﬁt order (NSs) to In require stars neutron (SBHs). (WDs), holes dwarfs black of white lar composed as distribution is such mass complexity remnants extended of unseen compact an layer dark of extra existence An likely the precession. by added node Lense-Thirring rela- and general precession pericenter for (prograde) of search the orbits—namely, a Keplerian inspire purely velocities to pericenter perturbations high tivistic The light. of percent few as remnants within compact physics In of detailed density the nuclei. stellar on the galactic as on well strongly of depend structure will sub-parsec rates EMRI of fact, understanding theoretical the clear as and such detectors Antenna ratio GW Space mass future extreme ometer with from (GWs) EMRIs) waves (henceforth gravitational inspirals of detection for prospects The disks of and ( center Galactic galaxies evidence the other observational in in formation further star is previous There of 2008). (Nayak- occurrence Rice, the clouds) and towards and two Bonnell of infall and collision 2007 the a al., from et (or resulting shin cloud starburst gaseous a a of via fragmentation formed subsequent have may it suggests clination aatcpae h oa tla ascnandi hsds swal constrained, weakly is the disk to this respect in with contained inclined mass probably is which stellar but 2009), total stellar al., The one et least plane. Lu Galactic- at and Galactic of 2006 the presence al., In the et for (Paumard clusters. disk evidence stellar observational ample than spherical is cuspy, richer there considerably of center, be models may simpliﬁed NSCs by of entailed content material and morphological The history. so evolutionary MBHs, common as a bulge had galaxy have host they the with likelihood than laws all younger scaling in often similar of are to thus stars obey also and younger NSCs The stars Myr. of formation. generations star several of complex episodes for very recurrent of evidence signs with show histories, They formation bulges. star galaxy of that values—from higher much . 10 4 ftegaiainlradius, gravitational the of . 10 o tr itiueaon asv lc hole black massive a around distribute stars How e.g. 4 M nM1 Gomn 03 edre l,20 n ei,2007). Levin, and 2005 al., et Bender 2003, (Goodman, M31) in

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5 ∝ ) M m 10 × = M ∗ • M 6 × 10 2 M • − 1 • M 10 / 2 − 3 /

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R b orsodn oa to corresponding − , 10 min 1 oi aeteeaestars are there case in so , ≈ steselrms den- mass stellar the is

∼ M 1pc T r h aiu and maximum the are r σ T

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i.e. (3) = oe esfrG science GW for News & Notes Notes & News for GW science 2 3My2,2010 21, May #3 T the to result, due eccentricity a by orbital given As its is change alone to orbital-averaged. emission object GW are mass stellar quantities the the for time that characteristic denote brackets the and ratio mass extreme with binary 1964) a (Peters, of to reduced case equations In Peters orbits. computed the formula Keplerian quadrupole GWs—assuming along Einstein’s emmited by the momentum approximated with well angular infinity sufficiently and is to latter away energy radiated orbital is of which secular loss that this with the describe equations equating Peters by will, MBH. process and the dynamical GWs towards of inspiral slowly emission dissipate result, will the it a through MBH, as momentum) a angular with system (and binary energy close orbital very its a forms object mass stellar a If eew mlctyasm h lse sisothermal, is cluster the assume implicitly we Here becomes mass MBH on timescale inside relaxation two-body dispersion of velocity dependence the the implies equation Jeans the Since at density stellar mean the and eoyfo h omto rcs n/rtelts togprubto) while perturbation); strong latest the and/or process formation the from memory 13 mass the in MBHs onto remnants compact of inspiral the range to sensitive be will LISA ecnld hthairbakhlsrsd nnce flwrdniy sarule a As density. lower with of MBH nuclei harboring in nuclei reside thumb, holes of black heavier that conclude We hnteiflec radius influence the then M GW • − − = 4Gyr 14 σ 10

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M e e sasm Bsi hsms ag olwthe follow range mass this in MBHs assume us Let . 304 64 2 15 5 ) • 5 r / h c r 2 5 T c h clsas scales a h G 5 ≈ rlx n 3 ∼ a G 3 (1 4 h 2 6 µ 3 (1 ∼ ∼ i M GM . µ red − 5 σ red • − WNotes GW × σ ρ 2 M M e 3 ∝ 10 2 2 • M e ρ ) M • 2 • 2 ∝ 7 σ ∝ ) 11 ∼ • 2 / r 5 & • 4 2 h 3 M / yr r , M / 2 − m 2 e 10 1 • 5 • 1

/ and / . 4 + µ M 1 2 7 . , M red + 24 73

( ! 304 121 r e ) have 2 = 10 + e const M 6 2 96 37 M • , T

e for , rlx 4 ! 2 r

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9 oe esfrG science GW for News & Notes Notes & News for GW science 10 WNotes GW d (DF) mass of tion MBH a with NSC a Consider e by set with those ihnteMHgaiainlptnilwell, potential gravitational MBH the Within DF the of knowledge energy specific of star (bound) each to sible stars of number The where E on depends cluster spherical with nucleus, Way Milky The steady-state. cl h energy the ical, potential gravitational To in oee,teganns fteptnilcetdb ag btfiie number finite) (but and large a by created potential N the of graininess the However, tion. object, compact a of capture or star MS a in of defined disruption be tidal can for cone, loss The hole. Φ aaini rvnb norltd ek w-oyecutr,teFokker-Planck the encounters, re- When two-body whole. weak, a uncorrelated, as by system driven the by is created laxation potential smooth mean, the on imposed where where Bne n rmie 08.I hslte ae h nerlaoesimplifies above integral the case, latter this In 2008). Tremaine, and (Binney v √ f 24 3 r ( 2 ( E x π Φ = fsaspoue at ml-cl utain htla oteso ifso of diffusion slow the to lead that fluctuations small-scale fast, produces stars of r sterda eoiy utemr,i easm niorpcD then DF isotropic an assume we if Furthermore, velocity. radial the is 0 d ) N , ( th GM 3 J J Φ = ρ ( v ) , E re,temto fsaseovsudrteiflec ftegoa,smoothed global, the of influence the under evolves stars of motion the order, ( i.e. ( E through r p T r of r , d ) ( • ) r J E Φ = ∗ ) ( ) = = − ( eaainrslsfo h neato ewe niiulprilssuper- particles individual between interaction the from results relaxation 3 E ) ( r = f E x ) M ) R 4 ( = 1 , − x π + Z ( = t / v 5 N • , r / 4 2 or ) v max Z 2 GM . v ( H R E ) E d pc by: space E 0 2 0 R o tr itiueaon asv lc hole black massive a around distribute stars How 3 − v r n t seic ria nua momentum, angular orbital (specific) its and , dr ) ie h rbblt ffidn trwti oueelement volume a within star a finding of probability the gives 10 ) n ria nua momentum angular orbital and max ( x esc 3 h aildniyprofile density radial The . Schw E • = / / d ( / 2 6 , ( r | 3 . E M r ) v Z J N v ) vv dv ) r J f stettlgaiainlptnildet h lse lsthe plus cluster the to due potential gravitational total the is rr dr o ahcs respectively. case each for |

Φ ( ( δ pc by space ≤ E E sterda eidfo pcne oprcne n back, and pericenter to apocenter from period radial the is d ( have ( E 3 ) , r 2 J 2 x J ) n h rvttoa potential gravitational the and lc p f − ) f d rae l h tr n h B.I h lse sspher- is cluster the If MBH. the and stars the all created ( ihenergy with , ( E Φ 3 x Φ Φ ( v ) , T x ( ( ( v r δ = , r r rlx ) ) v ) ) ( d E − r ) + − 3 < d nytruhtesa’ idn seic energy, (speciﬁc) binding star’s the through only x − E 1 p 1 d T / / Φ 3 = 2( 2 M 2 H v ( v Φ v codn oJasterm h Fo a of DF the theorem, Jeans to According . r − • n hudhv a iet eae noa into relaxed to time had have should and 2 ) 2 ( ∂ ) ttecne.Teselrdsrbto func- distribution stellar The center. the at + r E q δ = d M /∂ ) ( 1 E n nua momentum angular and J 4 − / • E π | − 2 > ρ ∼ E v ( Z p stefato fpaesaeacces- space phase of fraction the is 0 ) x r a 1 2010 21, May 2 4 ( 0 n h pe nerto ii is limit integration upper the and , ) ) E ≈ × × J Φ suiul eemndfo the from determined uniquely is f ) ( 10 fec traecntnso mo- of constants are star each of p ( r v ) E ∼ | 2 Ef dE ) 6 ) M GM f = √ ( 16

E 2 4 Φ ( π tnso h borderline. the on stands , , • E π ( J r ( ) GM r 2 ) d p ) , p = through 2( ( E 8 • Φ ) ) π J 3 f ( 2 E ( r = T J E ) − 5 ) − J / , | r x 2 srltdto related is , ( E E × and ) ) . f v ( f | E where , q = , ( J E ) , f

) ( (4)

E ∼ E ) oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 stoi,Fke-lnkeuto neeg pc sdfie,frec component each by 1990), for Weinberg, defined, and orbit-averaged, Chernoff is and time-dependent, space 1987 The energy (Spitzer, in equation description. Fokker-Planck its isotropic, for appropriate is equation a n hpr,17) Pels 92 a h rtt eonz htstatistical that recognize to first the was 1972) with Light- (Peebles, and clas- equilibrium, 1976 a thermal Wolf, 1977). is and Shapiro, MBH) Bahcall and 1972, (henceforth (Peebles, hole man dynamics black stellar massive in a problem around sical stars of distribution The 2.2 inadtegaiainpotential gravitation the DF operator- and the the This tion updating adopt 1990). successively Weinberg, we and in self-consistently, (Chernoff consists this and method do 1980) (Cohn, to by order outlined In method splitting updated. be to needs where equation, this In neeg pc,and space, energy in density stellar the As is hudhv eryiorpcvlcte.Teeoe fsasaealo h same DF the isotropic of form—an power-law all a are stars ra- takes stars disruption solution Nevertheless, tidal if quasi-steady the Therefore, the from obtain. mass, velocities. far would nearly-isotropic but have MBH, energy the should and of dius, field stars gravitational of the within flux well inward net (small) a radius acteristic at disruption tidal the to due either MBH equation Poisson’ from at rs.B ovn h oso qaina ecie,oei bet olwaccurately follow to able cluster. is stellar one the described, of as re-expansion equation slow Poisson the the solving convergence; By until so. iterations or several of of consists evolution step the since Poisson The q. invariant batic step, Poisson keep we step, R Schw acl ofCusp Wolf & Bahcall m r lentvl,b hsclcliin ewe tr niesm char- some inside stars between collisions physical by alternatively, or, ; ∗ = D 1 D Φ / EE Φ N ( E r ( , , o tr itiueaon asv lc hole black massive a around distribute stars How i i i r r ) , sarfrnems.Tegaiainlpotential gravitational The mass. reference a is coll × ) = = sudtdwiekeigteD xda ucino h adia- the of function a as fixed DF the keeping while updated is j xdwieupdating while fixed

u from run 4 − ebe lopeitdta,a eut taysaewith state steady a result, a as that, predicted also Peebles . µ µ p π 4 Φ ρ ( ρ i j 2 π E ( ! ( ( G r r 2 2 r ) ) ) G ) 2 ∂ X ∂ m vle vrtm,teselrgaiainlpotential gravitational stellar the time, over evolves N sso,ti tpi nydn teeyfiedfuinsteps diffusion five every at done only is step this slow, is 2 f t j ∼ c f i m ∗ 2 ( µ = " E ∗ 2 1 r q i 2 µ ) − ( − to ln i 2 E γ ∝ ∇ npyia pc.Teeepnnsaerelated are exponents These space. physical in , ∂ ln ) N Λ ∂ 2 F Z Φ e Φ E Λ E c − −∞ ( , ( i E E tenme fms components), mass of number (the r X r , /σ ) N ) dE j F c hog oso qain ntediffusion the In equation. Poisson through WNotes GW 2 = utb iltdsfcetycoet the to close sufficiently violated be must , E

, 0 f i 4 µ µ f ( = R π j E i ( j t E G ! ) − n h atr fsasb h MBH the by stars of capture the and Z 0 n h ifso ofcet.I the In coefﬁcients. diffusion the and ρ D ) E ( + r EE + ) ∞ Z . , f i E ∂ dE ( ∂ E + E f ∞ ) i 0 p − hog h ifso equa- diffusion the through dE ( E D 0 0 ) q E ( f f E j i ( , E 0 ) 0 f ) j . ( E Φ 0 ) # sdetermined is , µ i f = ( E m ) ∼ i Φ / m ( E r p ) ∗

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15 oe esfrG science GW for News & Notes Notes & News for GW science 16 WNotes GW E state, steady In tr ihsed ls oteecp velocity radius escape every the to close speeds not with was stars This BW a nucleus. real for a since in tion occur could they though even encounters—are strong to Ejections—due hr a enasrrsnl ml ubrof number small surprisingly a been has There afterwards. stable remaining 2004), al., et (Preto FP the of stars with lated dominated is uncorrelated, scattering that inher-by approximation—namely, assumptions (FP) report the Fokker-Planck to validating the ﬁrst thereby to the solution, ent Wolf were & 2004a) Bahcall al., the et of (Baumgardt alizations and 2004) al., et (Preto 2.4 eety oeo hmrpre h cuec fsrn assgeain (Hénon, segregation. mass strong very of until occurence and, 2006) the al., reported et them Freitag of and 2004b none recently, al., et (Baumgardt MBH a around tems reaches and grows cusp the as increases after MBH state a quasi-steady around a stars of density The mass. a was model starting density spatial of evolution where h rcino stars of fraction the ls none—ahrta h ihvlct jcino Ssa rmtecusp the from Figure star in a MS seen from be a result can of This might ejection 2003). object) Tremaine, velocity compact and (Yu high a the and star than MS encounter—rather a close between (or stars MS between nuclei, galactic as of high region as sub-parsec values the reach within can well dispersions that, Neverthe- velocity note ejections. also stellar should against one robust are less the cusps fact, stellar a this the in despite cusp that that the unambiguously from reassuring ejected is be It can stars time. of relaxation fraction non-negligible a that expect would are values these than higher velocity with v atparameter pact esc p L − N 3 -oyvalidation N-body / ( 2 α > + N 2 p F H tot 1 = v sahpremti ucin Taking function. hypergeometric a is esc const r ) = b F ≈ o tr itiueaon asv lc hole black massive a around distribute stars How 1 min r Since . E 2 F h ( 87% − bd nonesad npriua,dneselrcsspopu- cusps stellar dense particular, in and, encounters -body aigteDF the Taking . H H N γ a ea ml as small as be can ( R ) E R ( γ 0 = > 0 α hudb needn of independent be should ) v aemass same and v = esc ∝ esc 7 v p / esc ≈ L vv dv 1 vv dv m 4 v / → ) ≈ esc 0 L 2 ρ up tla este r eyhg n h rcinof fraction the and high very are densities stellar cusp, / . m N 6 ( 2 22 ennpol,wt B of MBH a with proﬁle, Dehnen / 2 1 r T H 2 tot ) / . rlx GM 4 f GM 6% n hs pc density space phase and and H ihvlct bv n ie fraction given any above velocity with r outaanteeto fsasfo h cusp. the from stars of ejection against robust are r tflosthat follows it , r ( ncoeareetwt ieclsdrvdfrom derived timescales with agreement close in • f • E ( epciey rm(uadTean,20)one 2003) Tremaine, and (Yu From respectively. − ) − E ≈ Z ) 2 1 2 1 ∼ E v ∝ 19% v + 2 2 ∞ 10 ( p E priori a p dE /σ /σ − /σ ihrthan higher 8 v pc 0 2 2 esc 2 p p ) p ( ( p ( a 1 2010 21, May N E r r ∼ rmtecs sas ut ag at large quite also is cusp the from ≈ p faB up ti ayt compute to easy is it cusp, BW a of ) E p 0 ) H bd tde fmlims sys- multi-mass of studies -body xlddfo h Pevolution, FP the from excluded ) sarsl,i clsas scales it result, a as ; 1 1000km R = f = → L hc ipasteF n NB and FP the displays which ,

( 1 E enn hsclcollisions physical meaning , 1 5 − 0 / ) / 4 0 N 4 = α f . hr are there 9 3 sbefore. as bd iuain show simulations -body ( / 2 const E v s 2 F esc otemnmmim- minimum the so , ) F 5% 1 priori a 1 (3 o oprsn The comparison. for if ; (3 / . ftettlcluster total the of / 2 2 p , , − ≈ − = p rva ques- trivial a p , 84% , 5 0 5 α N / ( / ;1) 2; γ bd re- -body ∈ 2; F fstars of [0 = α H 2 , ( ) 3 E 1]

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2 of ∼ ), oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 i.2 Fig. epciey h nta odto saDhe rﬁewt eta slope central with proﬁle Dehnen a is condition initial The respectively. 0 uvsaefo Bsmltos h asrtobtenhayadlgtsasis stars light and heavy between ratio mass The R simulations. NB from are curves fteitgain,after integrations, the of au.Tearw on oteradius the to point arrows The value. h ouin h smttcslope asymptotic The solution. the from decreases with MBH central a . 429 = ρ ρ

10 (r) (r) lwrpnl) orsodn otesrn n eksgeainregimes segregation weak and strong the to corresponding panels), (lower 10 10 10 10 10 10 10 10 10 10 10 h ubrfato fhaystars heavy of fraction number the ; asdniyproﬁles, density Mass -4 -2 -4 -2 0 2 4 0 2 4 6 10 -4 & 10 o tr itiueaon asv lc hole black massive a around distribute stars How 2 -3 to 5% ≈ -1.5 -1.5 10 ≈ ftettlms ftecutr h smttcslope asymptotic The cluster. the of mass total the of 7 Light, r (pc) -2 0 / 4 . 2 T hnmvn rmtesrn otewa rnhof branch weak the to strong the from moving when NB 10 FP ρ rlx L ( ( ∆ -1 r r h ) =0.08 ) γ lf aes and panels) (left mohcre r rmF acltos noisy calculations, FP from are curves Smooth . H 10 r h ≈ WNotes GW 0 and 3 / 2 10 0 f hogot rjs lgtyblwthis below slightly just or throughout, H . 1 -4 r = h . 10 2 . 5 -3 ρ × H ( 10 -2.1 -1.8 r 10 ) − rgtpnl)a h end the at panels) (right Heavy, 3 r (pc) -2 tppnl)and panels) (top NB 10 FP ∆ =13.2 -1 ∆ =0.08 10 γ 0 = 1 f H and γ = H

17 oe esfrG science GW for News & Notes Notes & News for GW science 18 WNotes GW ztoso h togms ergto ouinfrteselrdsrbto around distribution stellar the for Figure solution MBH. segregation a mass strong the of izations h ih opnn xedotto out extend component light the asymp- NB’s for branch, strong the in tendency, the slope is totic there although good quite is fun- was it well solution—as reasons, Bahcall-Wolf generalization—with these the Alexander-Hopman all of its For as validity the cusp. verify the systematically from as to stars question damental of not the in- ejection raised did against work an he robust Hénon’s but to are center. cluster, leads the globular spectrum at a whether MBH mass of to a core a of the of presence from the presence ejections include the stellar that of rate ago creased long shown has 1969) h ne est rfie ftehaycmoetdces steslto evolves solution when the branch ∆ as weak the decrease to component strong heavy the the from of profiles density inner the t clear time, first the for shown, have 2010a) Amaro-Seoane, and (Preto ∆ ∼ >> parameter ratio rdc lgtysrne assegregation. mass stronger slightly produce the for density space phase the stars, of light slopes and logarithmic heavy average The branches. 3 Fig. << 0 . 2 1 1 T , , R rlx

γ L H -0.2 0.2 0.4 0.6 0.8 1.2 H = H ( w rnhso assgeain ek( weak segregation: mass of branches Two r γ 0 1 1e-04 ed oeov oaqaised tt ls othe to close state quasi-steady a to evolve to tends h multi-mass 3 & L ) / ∆ rmF n Bcluain.Teareetbtenbt methods both between agreement The calculations. NB and FP from , ob lgtysalrta nF—o which FP—for in than smaller slightly be to 2 R h re/e uvs(P n ons(B orsodt mass a to correspond (NB) points and (FP) curves green/red The . h smttcinrdniysoe,i ohslto rnhs of branches, solution both in slopes, density inner asymptotic The . 2 = o tr itiueaon asv lc hole black massive a around distribute stars How ipastesaildniyproﬁles density spatial the displays 10 0.001 h gemn sqiego,ee huhN calculations NB though even good, quite is agreement The . tla up,otie rmteslto fteF equation, FP the of solution the from obtained cusps, stellar h p H i 0.01 and h p ∼ L i 0 safnto fteAeadr&Hopman & Alexander the of function a as , . 0.1 1 r h ncnrs,tehaycmoetshows component heavy the contrast, in ; ∆ ∆ sicesd sepce.I h ii of limit the In expected. as increased, is 1 N a 1 2010 21, May bd integrations. -body ∆ ρ 10 L > ( r γ ) 1 L and n tog( strong and ) , min 7 / 4 100 = ρ ouin hl for while solution, H 1 . ( 5 r ) h lpsof slopes The . tlt times, late at N 1000 bd real- -body ∆ <

1 ) oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 eo h limit the below that fsnl ascss hnfrthe for than cusps, mass single of for Furthermore, margin. branch, large strong very the the of a in that by broken compensate not are to although relations enough scaling not distribution—BW77 but branch, star’s weak heavy the to respect with expected slightly not are functions mass stellar have realistic since to slope, steep a such with galaxy rmF eut hw nFigure in shown results FP from say when especially = ∆ p tttsantrlepaaintelgrtmcslope logarithmic the explanation natural comparable, a become stitutes may densities the radius develops, some times, inside cusp late at steep nec- cusp; very not the neglect thorought is a and alone—and This when times lights all component. of at light approximation sea the accurate on an the essarily back-reaction on its friction and dynamical self-coupling its to dynamics both due the the assume is of essentially stars derivations one two heavy only these of of of both inspection fact, by In or terms. flux argument FP limits scaling asymptotic a the through overinterpreting either not this heuristically in at careful system single-mass be a should virtually one constitute stars light the though ital l h a to way the all virtually to branch, up weak only the extends on also slope branch: ymptotic solution the on depending behavior different a h gr htteslto sqaiaieydfeetdpnigo whether on depending different qualitatively from ∆ clear is is solution It the simulations. that NB figure from are the points while calculations, FP depen- the from the sured displays slopes It logarithmic ∆ average 2010b). the Amaro-Seoane, of dence and (Preto systems double-mass aino Figure of tation Figure branch, weak the in MBH); the with for events light the of that exceeds ii hr sawa eedneo h energy the on time; dependence with weak variation slight a some range is radial/energy show the slopes there on the (iii) slopes (ii) measured; the are of they dependence which some over is there (i) slopes: the of condition ofimteF acltosadvldt t neetasmtosa es nwhat in least the assumptions—at of inherent description its the broadly validate concerns results and NB calculations these FP detail, the quantitative confirm in differences some are there although L aaee—o h ae ihms ratio mass with cases the parameter—for > ∼ R 10 1 p 1 nthe In . H = / − 3 3 3 > 3 ∆ u,for but, ; p twudb airfrtelgtcmoett reach to component light the for easier be would it , umrzsterslso h xesv td fms ergto in segregation mass of study extensive the of results the summarizes H 1 f . / ( ∼ E 4 0 max weak . hogotadrahsavalue a reaches and throughout 0 01 . 5 3 083 ) R o tr itiueaon asv lc hole black massive a around distribute stars How h lpsfrtelgtsas ntesrn rnh loincrease also branch, strong the in stars, light the for slopes The . / R sta hr r oesucso netit ntemeasurement the on uncertainty of sources some are there that is = 4 branch, R = orsodn to corresponding 0 and eq 1 10 sipsdadas ntels oesz,i rsn.I sum, In present. if size, cone loss the on also and imposed is hssol aea feto h smttcsoe n con- and slopes asymptotic the on effect an have should This . hsitrrtto ol ml htfrlwrms ratio, mass lower for that imply would interpretation This . r h , ntesrn rnh h est ftehaycomponent heavy the of density the branch, strong the In . p p L L ∆ ∼ ∼ r > . 0 1 bulk 1 . / 1 0 10 W7saigrltosaevalid: are relations scaling BW77 , 3 elbelow, well , . nte atoaynt eadn h interpre- the regarding note cautionary Another . 01 p R rpriso tla distributions. stellar of properties H r h = ∆ ∼ ∼ adwl hrfr oiaeteinteraction the dominate therefore will (and WNotes GW 10 → 0 0 p . . 025 1 L aeti side h eutobtained result the indeed is case—this R 0 ρ r oeta ti eyulkl ofida find to unlikely very is it that Note . h H and = hl ntesrn rnhi extends it branch strong the on while , nthe In . 1 ρ > ≈ / 3 4 E and 1 p max o h same the for L H ( throughout. γ γ nteAeadr&Hopman & Alexander the on L H 10 twihteinrboundary inner the which at strong osntrahthe reach not does ≈ h mohlnsaemea- are lines smooth The . R 2 = . 5 when ) branch, γ 3 , L = ∆ p ∼ L 7 ∼ / 10 p ∆ ∆ 4 H ∆ 1 − characteristic / ∆ → ≈ ∼ 3 4 < However, . au even value 10 1 led at already 0 7 1 / / ρ ∆ esee we , 4 − derived γ 4 H 3 while , H < —still value sas- ’s ∼ 1 ρ or L

19 oe esfrG science GW for News & Notes Notes & News for GW science 20 WNotes GW n Bs( SBHs and nnme vrweebt for but, everywhere number in ratios mass several adopt we so constrained weakly also is SBHs especially, nertos h smttcsoeo Bsis SBHs 3 of slope asymptotic The integrations. value large slightly 10 and ilgo rmteisd-u.Adtie nlsso hseouinadipc on impact 2010b). and Amaro-Seoane, evolution and this (Preto of in analysis described detailed is rates A density EMRI the inside-out. dominate the SBHs from which over grow region will the so forms, cusp the after expansion density. aatcnce stphay(aese l,20) oi u xesv td fmass of study extensive values— our of in range so a 2007), al., adopt in et we IMF (Maness the segregation, indications heavy are top There is stars. nuclei high-mass of galactic IMF the to sensitive is remnants opnnsaeprotdt ersn D ( WDs 0 represent to purported are components salse after established Figure / . 6 2 , ein,ee huhM tr oiaei ubrtruhu h cusp. the inner throughout the number at in mass dominate have in stars SBHs dominant MS become The though they MBH. even result, regions, the a as around and, grown proﬁle fully steepest the has cusp the after components 4 Fig. ,Ms( MSs ), 15 hs itiuin r lal ntesrn ergto eie S dominate MSs regime. segregation strong the in clearly are distributions These . f , WD 20 4 R

hw h taysaedniypolso orcmoetselrsystem, stellar four-component a of proﬁles density state steady the shows ρ

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OLaye l,20) nti atclrcluain ehv dpe a adopted have we calculation, particular this In 2009). al., et (O’Leary 10 L eq -6 -4 -2 okrPac eut ih4cmoet.Teaypoi lpso all of slopes asymptotic The components. 4 with results Fokker-Planck 0 2 4 f -4 f 0 MS vle n nrae ntm stecutrudrosaso lblre- global slow a undergoes cluster the as time in increases and evolves BH . 11 = = PeoadAaoSon,21a 00) h asdsrbto of, distribution mass the 2010b); 2010a, Amaro-Seoane, and (Preto o tr itiueaon asv lc hole black massive a around distribute stars How ≈ 0 0 . . 007 873 0 . f 15 H (Light Stars) and -3 and T γ γ = =1.5 =2.1 (SBHs) rlx 0 optdwt P nti pcﬁ aclto,tefour the calculation, speciﬁc this In FP. with computed , R . R 007 BH MS r = nodrt aiiaetecmaio ihteNB the with comparison the facilitate to order in = . m -2 R 1 NS ,Ns( NSs ), eq / ∼ m log BH (3 10 r f − = BH f NS 4) 10 γ -1 f ∈ BH WD × .Tenme rcin fcompact of fractions number The ). = a 1 2010 21, May [10 10 0 ∼ = . − 01 − 2 3 3 0 . , 1 ≈ . and 10 11 while , 0 − . and 005 2 0 ] R , NS r f WDs NS h MSs BHs NSs R γ Bsdmnt in dominate SBHs , = WD WD ∼ m ∼ = (3 NS γ m / 1 − NS m WD 10) MS ∼ / m × γ = MS MS 10 R

1 .

− 4 = ∼ = 2 ) oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 ik a ulu,wudcrepn oruhyaHbl time. Hubble a roughly to correspond would nucleus, Way Milky reaching value lower Figure of panel top The 3 γ outeso up gis tla jcin n os u ofiec nteF de- FP the in confidence our the boost of and the ejections covered scription substantiate stellar range simulations against NB mass cusps agreement. the of good of robustness very representative in are are integra- that populations FP stellar masses and by more, NB evolution or between subsequent comparisons two, Detailed and with MBH. growth tions a the around from cusps outcome stellar robust of a is segregation Mass sasn rmteF vlto,bttesoe emt tblz around stabilize to seem slopes the but which evolution, noise FP numerical SBHs the to compo- that due from sign four fluctuations, clear absent are all a is There others, of center. the the all densities above to tempo- spatial out segregated stands the have the clearly depicts of SBHs panel the slopes of bottom that logarithmic The nents; components the the 3/2. of of below slopes evolution slightly the ral are as SBHs stronger the slightly qualita- than is is other double- segregation solution the NB in the as the that evolution—although, case, FP plot the mass the from obtained from one evident the to is similar It tively simulations. NB with puted MS falohrcmoet— intr fsrn assgeaini h nucleus. that the from in clearly segregation out mass strong stands of SBHs signature the components—a of other slope all of The scale. time relaxation a over 5 Fig. umr n discussion and Summary ∼ γ NS -oyrslswt opnns vlto ftelgrtmcslopes logarithmic the of Evolution components. 4 with results N-body ∼ 1 . 25 bulk o tr itiueaon asv lc hole black massive a around distribute stars How lhuhteW lp a oeidcto oeov eual to secularly evolve to indication some has slope WD the although , rpriso up rudMH.Wihrgm—ekor regime—weak Which MBHs. around cusps of properties γ WD 5 ∼ hw h est rfie ftesm oe,btcom- but model, same the of profiles density the shows 1 yteedo h nerto—hc,i cldt the to scaled if integration—which, the of end the by WNotes GW γ BH ∼ 2 ,

21 oe esfrG science GW for News & Notes Notes & News for GW science 22 WNotes GW o h hoiso aayfrain(ae ta. 08.Btseas Cleaiet (Callegari also see But 2008). a challenges al., from major et resulting the (Mayer of component formation 2010). one separate al., galaxy with a of connects not theories actually the This and for disk 2010). favor al., the to et of seem (Shen Bulge part merger Galactic is theo- the Bulge as of Galaxy, the data the Brunthaler,that kinematic of and stellar nature (Reid of pure-disk interpretations apparent motion retical the proper contradict SgrA* would the This a that from been 2004). fact has the constraints from there Way—aside strong that Milky are imply the likely involving there merger most major would recent be this less order would but or in possibility MBH, more Another formed binary center. be a Galactic is can the SgrA* IMBHs to that sufficient inflow that steady unlikely such very generate looks be to it can remnant sum, the In and 2009). lower is loss massive mass more metallicities, lower At star. Wolf-Rayet h tla betbigfre n h n euto uaa egri a is merger runaway a of result end of growth the the and limits formed severely being winds, object strong stellar very seems the to mechanism due such loss, metallicities, mass solar as of At inneficient mergers clusters. very runaway globular by of formed center be the to in hypothesized 2006), stars were al., IMBHs such et that Zwart fact the (Portegies of by proposed every been roughly at have core one IMBHs large a of carve inflow to order large in Such required be would IMBHs such of flow eswudtn oporsieywp u h tla up oee,tecr radius core is the event However, an cusp. such stellar encoun- by the body carved out three wipe through progressively stars to tend ejects would and stellar ters MBH the the in with mass of binary cores IMBH unequal-mass large an an of such inspiral of the formation instance, For the distribution. for mechanisms plausible devise to al., et Do and magnitude 2009 to al., down et complete (Buchholz Way be Milky to own 2009)—believed our of region sub-parsec ( the distribution in stellar initial the large in very present a dius unless be Amaro-Seoane, time, to two- Hubble postulated by and a is driven than core/hole (Preto nucleus—if shorter be type Way and to Milky expected 2010a) relaxation—are a body in Amaro-Seoane, growth cusp and for timescales (Preto 2010b), in shown As lhuhsc ti nymrial etrta n with one center, than the better towards marginally decreasing only density is stellar fit fits a a best with such the core although a constrained, slopes be weakly exclude could still to there seem is entail. data profile would counts density cusp number the segregated from strongly of a slope number the high the Although to respect with stars old that be could it Hopman be however, & to results; Alexander tend segregation nuclei galactic mass in Kroupa strong IMFs typical that a and IMF expects formation the one star on continuous IMF, depends Assuming nucleus population. particular stellar a its in of present is segregation mass strong—of & 2 c.Aayi ftenme onso pcrsoial dnie,odstars old identified, spectroscopically of counts number the of Analysis pc). ∼ o tr itiueaon asv lc hole black massive a around distribute stars How 260 M 10

∆ u naycs twl o oma MH(lbeke al., et (Glebbeek IMBH an form not will it case any in but , 7 > er,btta osntse eylkl nmr nlight in anymore likely very seem not does that but years, r 1 c ∼ n eksgeainwudensue. would segregation weak and 0 . 02 top-heavy c(amad ta. 06 n hsased in- steady a thus and 2006) al., et (Baumgardt pc nwihcs ti oelkl htthe that likely more is it case which in , a 1 2010 21, May > γ K 1 = Shdle l,20) and 2009), al., et (Schödel M 15 • . γ 5 ∼ rvasadfii of deficit a —reveals ∼ 10 1 3 / − 50 2 4 ti difficult is It . M i.e. or

htforms that 100 oera- core a ∼ 100 < γ larger.

, oe esfrG science GW for News & Notes Notes & News for GW science 3 3My2,2010 21, May #3 etri ae stepooiia ae u eetosrain eeln dearth a revealing observations recent Galactic But the and inside case. 2006b) giants prototipical stellar of the 2006a, the Alexander, as that and taken assume is (Hopman costumarily center state LISA steady by in rates are Es- detection 2007). cusps al., and et event Amaro-Seoane and for SgrA* 2005 timates of Alexander, MBHs and for (Hopman precisely below LISA and by mass detectable be will remnants compact of EMRIs n 3) oeo h iuain eedn tteTfsencutro h AEI. the of cluster Tuffstein the at done were 823.219-439/30 simulations (Az: the Baden-Württemberg of of Some Min- Arts /36). the the and by and and Research Foundation Volkswagen Science, the of of istry 041-043 I/80 project by funded was RC:sehttp://www.ari.uni-heidelberg.de/grace see GRACE: RP-Acutr tteAtooice ehnIsiu nHeidelberg in high-performance Rechen-Institut dedicated the Astronomisches on the out at carried Raum- clusters und been Luft- GRAPE-6A have für simulations Zentrum The (Deutsches DLR by fahrt). supported partly was work This Fi- José Alexander, Tal Amaro-Seoane, Spurzem. Rainer Pau and with estas discussions from beneﬁted have I Acknowledgements the as such system, the of for mass. properties the MBH framework on central theoretical rates more general EMRI be of a will dependence develop the detections 2010) exploring LISA al., is which et nucleus from (Amaro-Seoane Way nucleus Milky frequent. the The of prototype cusps. the stellar necessarily segregated from originate will events are around peak to expected are pe ato h asrne,snecs rwhtm clscnsilb ut long quite be still the can in scales time MBHs growth with cusp since nuclei ( range—, for existence mass the the possibility—especially of time, a part Hubble remains upper a still than nuclei less in cored re-grow of may cusps stellar Although mon. e.g. . 6 1 y nMlyWytp uli.Hwvr ic MIdtcinrtsb LISA by rates detection EMRI since However, nuclei). type Way Milky in Gyr y for Gyr M 1 o tr itiueaon asv lc hole black massive a around distribute stars How • cfrom pc . 1 . 2 × SgrA 10 M 6 M • ∗

∼ n as h osblt htcrdnce r com- are nuclei cored that possibility the raise and esilepc htasbtnilfato fEMRI of fraction substantial a that expect still we , 4 × 10 WNotes GW 5 − 10 6 M

Gi,20) n egot times re-growth and 2009), (Gair, 3 which , not

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, , oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 hpr,S 18) ot al iuain fte2+1dmninlFokker-Planck dimensional 1 + 2 the of simulations Carlo Monte (1985). S. Shapiro, u .adTean,S 20) jcino yevlct tr yte(iay Black (Binary) the by Stars massive Hypervelocity of of Ejection growth (2003). S. on Tremaine, and constraints Q. Yu, Observational (2002). S. Tremaine, and Q. Yu, (1987). L. Spitzer, quasars. of (2010). Masses (1982). al. A. R.et Soltan, Propris, De and D. C. Howard, J., Kormendy, M., R. Rich, J., Shen, oei h aatcCenter. Galactic the in Hole holes. black p.. 191 1987, Press, University Formation. Galaxy for Challenge A – Galaxy e-prints Pure-Disk ArXiv a as Way Milky Our In holes. black central clusters massive, star containing of clusters Dynamics star Spherical - equation o tr itiueaon asv lc hole black massive a around distribute stars How MNRAS yaia vlto fgoua clusters globular of evolution Dynamical . 335:965-976. , ae 372-412. pages , srnmclJournal Astronomical MNRAS WNotes GW 200:115-122. , 599:1129-1138. , rneo,N,Princeton NJ, Princeton, .

27 oe esfrG science GW for News & Notes Notes & News for GW science 28 WNotes GW Eprint: Authors: Data LISA Bursts Mock Gravitational-Wave in Cosmic-String for Searches Authors: Binaries Spin- Compact General order of Dynamics next-to-leading Squared for Hamiltonian Reduced distri- the derive we and frequencies sev- problem, cut-off search elucidate of this and bution in identify imbedded also are We emitting that impossible. the symmetries practically eral of be location often sky will correct the loop inferring string LISA) (for ﬁtting why waveform illustrate psi, matically the of (A expect maps over LISA’s can draw [maximized understand LISA we To factor sources, accurately sources. string-burst how for string-burst calculate resolution of We angular parameters physical psi. the incorpo- and measure that A to F-statistic on the priors of realistic version rates Bayesian times we approximate, arrival likelihood; an the burst maximizes demonstrate over that also quickly statistic frequentist search a to essentially FFT is F-statistic the dard use and polarization, and psi, amplitude and signal’s A the use over implementations maximize our analytically to space, F-statistic search the the of respectively. versions dimensionality packages, two effective software The the PyMC reduce and Challenges. To MultiNest Data available LISA publicly Mock the the on of rely context developed the have on within we tested report that pipeline and we search string-burst both Here LISA-oriented by a cosmic- of detectable on versions interferometers. be two develop gravitational-wave could generically that space-based that radiation and cusps gravitational ground- the of bursts so, emit If loops string universe. early the in formed Abstract: algorithms search timation; Keywords: http://arxiv.org/abs/1002.4153 oe,McalI;Cte,Cr;Vlinr,Michele Vallisneri, Curt; Cutler, I.; Michael Cohen, eg,See;Senof a;Shee,Gerhard Schaefer, Jan; Steinhoff, Steven; Hergt, ewr fosral,mcocpccsi spr)tig a have may (super-)strings cosmic macroscopic observable, of network A uss aaaayi;g-c erplsHsig;MD;prmtres- parameter MLDC; Metropolis-Hastings; gr-qc; analysis; data bursts; o tr itiueaon asv lc hole black massive a around distribute stars How coe 09t ac 2010 March to 2009 October f max eetdabstracts Selected t C o bevbebursts. observable for ]a ucino k oiin hs asdra- maps these position; sky of function a as )] a 1 2010 21, May

C h stan- The . oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 t.Cmaio ihanneue oeta acltdwti h fetv Field Effective the brack- within Poisson made. calculated is canonical potential approach of nonreduced Theory terms a spin, with in for Comparison given motion are of ets. equations variables corresponding momentum The and position equations. field Einstein’s the- perturbation of order self-gravitating ory post-Newtonian with spin-induced second account binaries in into effects of taking deformation kinds stars quadrupolar neutron all Hamilton- and/or of holes The dynamics black like spin components presented. the to is applicable binaries order is compact next-to-leading ian the general for of condition) dynamics supplementary spin-squared spin eliminated with (i.e., Abstract: Keywords: Eprint: Msse nue eoac ihfnaetlfeuny1yr the 1 of frequency pulling fundamental gravitational with periodic resonance the a that induces show system We EM masses. test LISA of motion Abstract: Keywords: Earth- the Authors: to due orbits system free-fall Moon LISA of Modulation Authors: Recoils Hole Black of Suppression Relativistic synodic the of harmonics integer 10 (9.92 to month equal frequencies with perturbations periodic Eprint: M. Sereno, A.; Ortolan, G.; erfil ol rvd naslt airto o h IAsniiiya eylow very col- at gravitational sensitivity data system LISA Doppler EM the the for the calibration that in frequencies. absolute suggests detected an This provide be could mission. can field near space system LISA EM 10 the to the by down of lected extrapolated harmonics as few curve, a respectively. sensitivity harmonic, finding that LISA 6th couple, and the 2nd take masses the we for test 10pm If each and 3mm between between motions range they relative that the on harmonics) 6th http://arxiv.org/abs/1002.2093 http://arxiv.org/abs/1003.5528 edn ihe;Sehk,Urc;Bri Emanuele Berti, Ulrich; Sperhake, Michael; Kesden, edno . eMrh,F;D iti . ezr . azr,F;Mazzolo, F.; Marzari, P.; Jetzer, R.; Pietri, De F.; Marchi, De M.; Cerdonio, ecluaeteefc fteErhMo E)sse ntefree-fall the on system (EM) Earth-Moon the of effect the calculate We ihnteps etna rmwr h ul eue Hamiltonian reduced fully the framework Newtonian post the Within sr-hH;g-c otNwointer;spin theory; post-Newtonian gr-qc; astro-ph.HE; eetr;goei oin rq;interferometers gr-qc; motion; geodesic detectors; − 7 o tr itiueaon asv lc hole black massive a around distribute stars How z.W hneaut h fet fteeprubtos(pt the to (up perturbations these of effects the evaluate then We Hz). WNotes GW − − 1 6 n eisof series a and z eobtain we Hz,

29 oe esfrG science GW for News & Notes Notes & News for GW science 30 WNotes GW ai f91.Ti euto ilgetyices h rcino aaisretaining galaxies of fraction mass the a increase with holes. greatly black holes will supermassive black their reduction spinning median This maximally the for 9/11. reduces km/s of paper 273 ratio this to km/s in 864 discussed from alignment recoil spin the distributed, ically eue h eolvlct vni h bec fgs o xml,i h nl be- angle the if example, For gas. significantly of alignment absence This the other. in tween each even velocity with scales recoil spins sub-parsec the hole on reduces black precession binary spin the relativistic align L, can momentum angular orbital the neti crto osna h iaybakhls nti etr eso that show we Letter, this In holes. spin black the binary if the the near in highly flows produced on depends accretion angu- hole alignment uncertain black orbital this final of their effectiveness the with the However, of spins merger. velocity subsequent hole recoil black the binary reducing the momentum, lar align can than less disk most much circumbinary that at velocities a holes paradigm escape black the having supermassive challenges despite retain This centers yet their binary. mergers, initial hierarchical through the form of galaxies mass of center the to nabnr egrcnrci ihavlct pto up velocity a with recoil can merger binary a in Abstract: relativity numerical holes; black of Keywords: Eprint: nertr hc a erie oabtayodrb opsto.Afourth-order A composition. by order arbitrary to raised time-reversible symplectic, be a can is the outcome which of The integrator, terms motion. structure individual of equations special the underlying the integrate the exploiting to of analytically, possible Hamiltonians is contributions. spin-spin it spin and splitting, and spin-orbit the orbital of of flows context the the combine In we approach binary. splitting black-hole a spinning Using a of motion post-Newtonian the computing numerically Abstract: spin theory; post-Newtonian relativity; numerical methods; Keywords: Eprint: Authors: Spin with of Motion Equations Post-Newtonian of Integration Symplectic S http://arxiv.org/abs/1003.5122 http://arxiv.org/abs/1003.4993 1 n tlresprtosi 0dgeswietescn spin second the while degrees 10 is separations large at L and uih hita;Wlhr en;Bugan Bernd Bruegmann, Benny; Walther, Christian; Lubich, epeetanncnnclysmlci nerto ceetioe to tailored scheme integration symplectic non-canonically a present We ueia-eaiiysmltosidct httebakhl produced hole black the that indicate simulations Numerical-relativity S sr-hC;g-c rvttoa eol ik/eol asv binaries massive kicks/recoil; recoil; gravitational gr-qc; astro-ph.CO; 1 rq;msiebnre fbakhls ahp;mt.P numerical math.MP; math-ph; holes; black of binaries massive gr-qc; ftemr asv iaybakhl see atal lge with aligned partially even is hole black binary massive more the of o tr itiueaon asv lc hole black massive a around distribute stars How a 1 2010 21, May v max ∼ 4 , 000 v max mswt respect with km/s neato with Interaction .

2 sisotrop- is oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 ttecnr fNC68.W ics h netite fti pe ii n the and limit upper this of of analysis. mass uncertainties hole the discuss black We suggested 6388. previously NGC upper of an centre place the we at mass, hole be- black cluster. relationship of a and the limit is in luminosity which sources radio holes X-ray centre luminosity, black Chandra cluster X-ray accreting the the tween of of at plane any uJy) fundamental the 27 the of on of locations Based level the noise at r.m.s. or a gravity (with there of that detected show source We radio 6388. NGC no cluster is globular the of (ATCA) Array Compact scope to due equations. forces post-Newtonian dissipative full weak of the prop- presence in the Favorable damping in radiation retained simulations. are long-term integrator in the conserva- of momentum erties and angular growth and error energy concerning of behavior excellent tion give to shown is version ftruec.Ulk rvosaaye fti rbe,orrslsd o depend not decay do results to our due problem, lost this energy of due and analyses equilibrium previous accretion energy Unlike by and that turbulence. released instability curve of energy rotation gravitational between arbitrary marginal balance an of the with state to stars a and in gas kept of is disk axisymmetric thin a ing Abstract: Keywords: Eprint: Authors: Disks Instability- Dominated Gravitational of Evolution and Dynamics the On Abstract: observations Keywords: Authors: the hole on black limit central upper its of an mass 6388: NGC of observations Radio Eprint: B. Lanzoni, http://arxiv.org/abs/1003.4513 http://arxiv.org/abs/1003.4604 1500 rmoz akR;Bret Andreas Burkert, R.; Mark Krumholz, epeetaﬁs-rnilsdrvto fteeouineutosdescrib- equations evolution the of derivation ﬁrst-principles a present We epeetterslso eprdoosrain ihteAsrlaTele- Australia the with observations radio deep of results the present We sh . art . obl . odn,E;Cra,M;Tiui,A.; Tzioumis, M.; Coriat, E.; Kording, S.; Corbel, P.; Kaaret, D.; Cseh, sr-hG;atop.E srpyis nemdaems lc holes; black intermediate-mass astrophysics; astro-ph.HE; astro-ph.GA; crto ic;atop.O sr-hG;astrophysics astro-ph.GA; astro-ph.CO; discs; accretion M

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31 oe esfrG science GW for News & Notes Notes & News for GW science 32 WNotes GW ihrdhf aais h ue aeu ik flclglxe,adaceindisks accretion and galaxies, including local environments, of of disks protostars. range around gaseous broad outer a the in of galaxies, implications disks redshift to the of high comparable discuss structure we timescales Finally, the on for high. it is results rate into these accretion evolve the disks will if that period state show orbital We steady rota- the edge. of the disk out fraction, the initially onto mass accretion are gas external that the of rate of the function and a curve, tion as mass transport of momentum rates and angular density, surface and state dispersion, this velocity in con- the disks steady-state determine for a analytically and instability, is we gravitational there by that dominated show disks We for equations. figuration dynamical fluid transport the time-dependent from and rates position- the determine to self-consistently due we argument. transport equilibrium Instead, momentum energy angular order-of-magnitude and an mass on of or instability, rate gravitational the for model assumed an on Keywords: Eprint: Authors: Holes Black Supermassive of Formation the against well compares waveforms fur- resultant mass-ratios the case. with of damping used analysis constant be Our to one. damping from the providether for and forms plays, un- damping non-constant of this calculation found explicit, role the been two the for carefully has sim- needed examine We are it Such binaries. factor However, mass damping factor. equal the damping. of damping values for a specific value very includes constant that which a driver, use gamma typically a ulations of use make holes Abstract: waveforms holes; black sive Keywords: Eprint: Authors: hole black mass binaries unequal for condition shift Dynamical http://arxiv.org/abs/1003.4404 http://arxiv.org/abs/1003.4681 ootr,Marta Volonteri, Bernd Bruegmann, Jason; Grigsby, Doreen; Mueller, eti ueia rmwrsue o h vlto fbnr black binary of evolution the for used frameworks numerical Certain sr-hC;csooy uemsiebakholes black supermassive cosmology; astro-ph.CO; rq;msiebnre fbakhls ueia eaiiy supermas- relativity; numerical holes; black of binaries massive gr-qc; o tr itiueaon asv lc hole black massive a around distribute stars How

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 pcs n osbeosrainltsso hs scenarios. cosmic these early of at tests place observational to likely possible are and black that epochs, discuss holes will black I ‘seed’ for population. are processes hole that formation black processes hole massive physical the the of of evolution the some to here with conducive review galaxies briefly substantial I of proto- buildup wells? the small potential await in deeper of to efficiency hundreds had same formation in their the up did split with or was form galaxies, it seeds when MBH stage Did the to components. back single smaller traced a be cosmologies, can hierarchical In today galaxy structure. big galactic of evolution the to linked are Abstract: icvr fFu p-cl iayAGNs Binary kpc-Scale Four of Discovery space. parameter kick the two of the aspects because different only astrophysical explored any was sets for conflict data apparent enough previous good fit the is can This that we shows %. that and 5 show calculation, than we from better to remnants kick, data merged out-of-plane existing out-of-plane eject the all for thus the almost ansatz can only different and is a km/s to it Using 500 fit because galaxies. than good resolve more reach a to can important each that is kick, kicks This out-of-plane dominant for- sets. conflicting the data apparently for different time, proposed some been for have understood mulae been has holes black lescing Abstract: relativity numerical holes; black of Keywords: Eprint: J. Bernard Kelly, D.; Authors: Wave Gravitational Hole Black Kicks for Formula General A Keywords: Eprint: Authors: rpriso h otglx uha ug asadvlct iprin These ( host dispersion. the than velocity massive and less and mass much mass while bulge MBH MBHs, as central the such that between suggest galaxy results relations host of the number of a properties established also have Studies in;sprasv lc holes black supermassive tions; http://arxiv.org/abs/1003.3865 http://arxiv.org/abs/1003.3467 i,Xn ree en . hn u;Srus ihe A. Michael Strauss, Yue; Shen, E.; Jenny Greene, Xin; Liu, a ee,JmsR;Mle,M oea;Bkr onG;Bgs William Boggs, G.; John Baker, Coleman; M. Miller, R.; James Meter, van lhuhtegaiainlwv ikvlct nteobtlpaeo coa- of plane orbital the in velocity kick wave gravitational the Although vdnesosta asv lc oe eiei otlclgalaxies. local most in reside holes black massive that shows Evidence sr-hH;g-c rvttoa eol ik/eol asv binaries massive kicks/recoil; recoil; gravitational gr-qc; astro-ph.HE; sr-hC;atohsc;msiebnre fbakhls observa- holes; black of binaries massive astrophysics; astro-ph.CO; o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW ∼ 0.1%),

33 oe esfrG science GW for News & Notes Notes & News for GW science 34 WNotes GW fol 3ojcs eosrtn h fcec fti ehiu ofidkpc-scale find to technique sample this a from of efficiency drawn were the AGNs. objects demonstrating binary These line-of-sight objects, with 43 km/s. bulges, show only hundred stellar of spectra few stellar the slit a double with of optical and coincident offsets while spatially velocity features kpc, nuclei tidal several 2 reveal of Seyfert images separation four two projected NIR the for a the scenario with system, SMBH bulges each binary the In support and strongly m objects. telescopes 6.5 m Magellan the 3.5 from near- APO obtained Deep spectra the SMBH. slit single optical a and around images gas (NIR) could region infrared narrow-line or merger, of galaxy motions result bulk a to could in due peaks (SMBHs) be double holes The black supermassive spectra. active fiber pairing their from double-peaked in on lines based emission Survey 4959,5007 Sky III] Digital [O Sloan the from selected originally were Abstract: forseai soei hc h rsn nemdaems lc oe(IMBH) hole black intermediate-mass present the which in one outcome the is phase, scenario formation small SG and our the ac- mass of of the hole duration determining black the seed in a in near-universal important to variations a are cluster-to-cluster up Assuming dynamics by growth. gas mass hole the hole black of seed black tual details pre-existing the The increase a can onto 100. accretion of accretion gas factor significant that to show We that lead show also hole. we ultimately black can Letter densities, this density In high gas stars. reaches high SG gas the of the hydro- in subsystem where of concentrated collect core, centrally ejecta means a cluster AGB by forming the study, the in previous that flow shown a cooling have In a we gas. simulations, have this N-body stars and of (AGB) dynamical source Branch in- the Giant formed, as Asymptotic proposed have high-temperature massive been the must through First-generation stars processed these matter cycle. which contain CNO must of (SG) gas out the second-generation gas that of of dicating sources abundances the chemical constrain age The uniform stars of stars composition. of chemical composed that populations" and paradigm stellar common "simple the are challenging clusters globular populations, stellar multiple host clusters Abstract: Keywords: Eprint: Francesca D’Antona, Authors: Clus- Globular ters Early in Holes Black Intermediate-Mass http://arxiv.org/abs/1003.3470 erpr h icvr ffu p-cl iayAN.Teeobjects These AGNs. binary kpc-scale four of discovery the report We pcrsoi n htmti bevtosso htmn globular many that show observations photometric and Spectroscopic eprn,Erc;MMla,SehnL . ’roe Annibale; D’Ercole, W.; L. Stephen McMillan, Enrico; Vesperini, sr-hG;goua lses MI nemdaems lc holes black intermediate-mass IMRI; clusters; globular astro-ph.GA; o tr itiueaon asv lc hole black massive a around distribute stars How

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 ai rsne rvdsantrlmcaimfrtefraino nIB tthe at IMBH phase. an star-formation of SG the formation sce- during The the center for properties. cluster mechanism cluster natural current a the provides on presented dependence nario weak a only have may mass cin.Rttoa eomto ftecmatojcsi noprtd o arbitrary For incorporated. is objects compact the inter- of spin-orbit deformation order ob- Rotational next-to-leading is actions. and binaries spin-spin compact order spinning leading for including motion tained of equations accurate (PN) Newtonian Abstract: forms Keywords: Eprint: Authors: spin order higher under coupling momentum angular and aligned spins with binaries compact of motion orbital Eccentric LISA. with memory the and of ringdown); detectability merger, in- the (inspiral, that of coalescence estimates memory hole realistic nonlinear black (3) binary the of of phases calculations all third ﬁrst clude to the waveform the (2) contri- completing order); memory (thus post-Newtonian amplitude the waveform of inspiral computations the (1) to including: bution memory work, current nonlinear recent from and some extracted linear summarize easily the I not reviewing is After memory simulations. relativity nonlinear (Newtonian-quadrupole) numerical the leading fact, at this starting Despite amplitude nonlinear order. the signal Surprisingly, passed. the has affects wave the memory after displacement persists that permanent masses a test the causes in- of memory gravitational-wave with ideal an gravitational-wave In a waves. waves terferometer emitted previously gravitational the from by originates sourced It are that amplitude. gravitational-wave the to bution Abstract: forms Keywords: Eprint: Authors: effect memory gravitational-wave The http://arxiv.org/abs/1003.2735 http://arxiv.org/abs/1003.3486 ese,Mne;Hrug oans cafr Gerhard Schaefer, Johannes; Hartung, Manuel; Tessmer, Marc Favata, h olna eoyefc sasol-rwn,nnoclaoycontri- non-oscillatory slowly-growing, a is effect memory nonlinear The us-elra aaeeiainfrtesltoso eodpost- second of solutions the for parameterisation quasi-Keplerian A rq;msiebnre fbakhls otNwointer;wave- theory; post-Newtonian holes; black of binaries massive gr-qc; sr-hH;gnrlrltvt;g-c otNwointer;wave- theory; post-Newtonian gr-qc; relativity; general astro-ph.HE; o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW

35 oe esfrG science GW for News & Notes Notes & News for GW science 36 WNotes GW Eprint: Authors: A* Sgr of Nature Underluminous The contri- spin-spin order. 1PN 0PN and of orbit counted spin are spins 1.5PN or- the particle, where the point in butions, to 2PN given are anti-parallel to forms or up wave form parallel gravitational analytic be emitted The to vector. taken momentum are angular bital orientations spin the ratios mass Authors: binary of merger holes the black in "anti-kick" the Understanding accretion the cross to photons flare IR for taken time upscattered. optically being the of before expansion to flow adiabatic but to the plasma, due between NOT hot predicted X-rays, is thick and minutes near-IR of the tens to in for minutes flaring account of peak pho- can delay emission flare time submm A X-ray IR the flares. of of X-ray for the (ICS) responsible Modeling electrons scattering energetic Compton mechanism bands. the inverse emission by wavelength tons that the different suggests to in flares related activity near-IR is flare and issue of other under- cause the The the explain then part A*. and could in Sgr which Sgr can of feedback factors from nature a uncertain luminous outflow as These act to rate. then accretion lead could Bondi A* could reduce Sgr sub-relativistic. plasma from be outflow the to Significant estimated of A*. is of motion plasma expansion bulk the adiabatic of relativistic of speed context However, expansion the The in of understood picture plasma. be delay hot time can recent emission feed- the flare Furthermore, gas ionized peak rate. of Bondi the momentum the accu- angular lower estimating could net in A* A factor Sgr A*. critical ing Sgr a orbiting unto be from could rate winds A* accretion stellar Sgr the orbiting ionized rately disks the two of or one momentum counterparts. in angular massive stars luminosity the more issues: bolometric its that important of out its those two turns with than It address less A* magnitude to Sgr of order orders of several in nature being out underluminous carried the been concerns has one A* Sgr hole black Abstract: holes black Keywords: http://arxiv.org/abs/1003.1519 ue-ae,F;Wrl,M. Wardle, F.; Yusef-Zadeh, ezla uin;Mcd,RdioP;Jrmlo oéLuis José Jaramillo, P.; Rodrigo Macedo, Luciano; Rezzolla, ntels eea er,anme fosrigcmagso h massive the of campaigns observing of number a years, several last the In sr-hG;atohsc;osrain;SgtaisA;supermassive A*; Sagittarius observations; astrophysics; astro-ph.GA; o tr itiueaon asv lc hole black massive a around distribute stars How

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 Keywords: Eprint: ae ftedpnec ftesatrn hehl ntebakhl pnadon and spin hole black the on spacetime. threshold the esti- of scattering qualitative dimensionality the provide the of to dependence analogy to the geodesic attention of a particular mates use paying also and We radiation hole, the regime. plunging black near-critical of particle the Schwarzschild structure point a multipolar a into the by explore parameter holes the we impact In black and the parameter. energy impact of arbitrary ﬁnite one with limit" with replace "zero-frequency particles we a point calculation by two radiation second of the collision estimate the from we of calculation extracted analysis ﬁrst spectra calcula- the energy gravita- semianalytical In the complementary emitted tions. two of the using features and simulations many collisions relativity explain these numerical We of nature semianalytical radiation. use the tional we understand paper this better In to relativity. general tools of nonlinearities the study to Abstract: relativity numerical holes; Keywords: Eprint: Nicolas Yunes, Ulrich; Sperhake, Frans; torius, Authors: en- hole counters and black ultrarelativistic thresholds in radiation scattering gravitational of estimates Semianalytical a oadee nesadn ftennierdnmc fbakhl spacetimes. the black-hole of opening dynamics thus nonlinear gauge- the binaries, of a hole understanding qualitative deeper black in the a inspiralling all to radiated way provides of momenta setup features simpler and quantitative this also energies time, but same the the both At measure manner. invariant to spacetimes Robinson-Trautman us of the properties allows the of and on intensity focussed and is direction analysis the Our determines recoil. horizon anisotropic the intrinsically the on in where understood distribution hole black easily curvature deformed be a can from anti-kick radiation ex- the the of that and terms show We investigated yet not explanation. been has simple merger, have the a after found process deceleration sudden this the namely of "anti-kick", the aspects plained, numerical-relativity many of While results exciting most calculations. the of one represents holes black binary Abstract: relativity numerical http://arxiv.org/abs/1003.0873 http://arxiv.org/abs/1003.0812 et,Eaul;Croo io;Hnee,Tna eo,Mdln;Pre- Madalena; Lemos, Tanja; Hinderer, Vitor; Cardoso, Emanuele; Berti, lrrltvsi olsoso lc oe r da eaknexperiments gedanken ideal are holes black of collisions Ultrarelativistic h eeaino ag eolvlct rmteisia n egrof merger and inspiral the from velocity recoil large a of generation The rq;gaiainlrci;kcsrci;msiebnre fbakholes; black of binaries massive kicks/recoil; recoil; gravitational gr-qc; eea eaiiy edscmto;g-c asv iaiso black of binaries massive gr-qc; motion; geodesic relativity; general o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW

37 oe esfrG science GW for News & Notes Notes & News for GW science 38 WNotes GW naceigbakhl nti eryLNRgalaxy. of LINER presence nearby the this suggest in do hole black ratios accreting line an emission hydrogen molecular AGN-like and of mass mass-to-light hole constant black a a suggests Assuming modeling dynamical profile. stellar un- mass by the stellar hindered ratio, is central hole the black of in mass mass intermediate cluster certainties possible star a nuclear of total detection a mod- gives Dynamical Dynamical kinematics stars. stellar older the much of by eling dominated is bulge of of the half ages while with having merger), cluster distinct, galaxy star also nuclear are the components of three mass the the the of of that populations to Mol- stellar orthogonal rotation excess. nearly The rotation central modest stars. with the disk with in a kinematics seen traces counter-rotation emission distinct hydrogen and ecular cluster have cluster star components the nuclear within the These excess in light seen pc. central a <3 and radii cluster, com- star three at the nuclear of in presence a only the possible bulge, suggests detail a profile of ponents, level brightness a surface at The nucleus galaxies. 404 nearest NGC the near- of obser- assisted study These enable optics imaging. vations adaptive HST of and spectroscopy, combination optical a spectroscopy, using integral-field IR 404 NGC galaxy S0 nearby in Abstract: observations Keywords: Eprint: McDermid, P.; Victor Debattista, Andrew D.; Stephens, Robert Thomas; Blum, Puzia, Richard; Knut; Olsen, Nate; Bastian, son; Authors: Inter- Possible Hole and Black Cluster Mass Star mediate Nucleus: 404 NGC The Eprint: Authors: canoni- through order coordinates in post-Newtonian rest-frame higher Hamiltonian and hole center-of-mass cal black spinning Binary mass with hole black a by fit best are of kinematics gas hydrogen molecular the while 4 . 5 × 10 http://arxiv.org/abs/1003.0390 http://arxiv.org/abs/1003.0680 oh,Tla . cäe,Gerhard Schäfer, J.; Tilman Rothe, 5 eeaietencermrhlg,knmtc,adselrpopulations stellar and kinematics, morphology, nuclear the examine We eh nlC;Cpelr,Mcee emyr aie adel Nel- Caldwell, Nadine; Neumayer, Michele; Cappellari, C.; Anil Seth, M sr-hC;atop.A srpyis nemdaems lc holes; black intermediate-mass astrophysics; astro-ph.GA; astro-ph.CO;

neovdadpsil aibeds msini h near-infrared the in emission dust variable possibly and Unresolved . o tr itiueaon asv lc hole black massive a around distribute stars How a 1 2010 21, May ∼ y prasrsligfo a from resulting (perhaps Gyr 1 < 1 . 1 1 × × 10 10 7 5 M M

. , oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 euircutr h etfi oe oteknmtcdt ed,mroe,t cluster a this to moreover, for leads, data status kinematic non-relaxed the to a model of fit the best thought in The current cluster. than the peculiar segregation confirms mass This without better case. is segregated that profile dispersion velocity sight 5 Abstract: Keywords: eut.B h aaercfitn ftemdlt eetHTASdt o the for data HST/ACS recent of ratio to mass total model cluster to the IMBH an of found we fitting profile, brightness parametric surface the By the including by Results. model King the vicinity. IMBH of the generalisation veloc- in a anisotropic function distribution in with Bahcall-Wolf consists model It spherical distribution. self-consistent ity a employed We mass. in Methods. its IMBH of an estimate of presence independent the an to providing support at further and giving Centauri at omega aim we paper, this In Aims. formation. galaxy astrophysi- and current stellar in in topic implications controversial important and with hot research at a cal (IMBHs) is holes clusters black globular intermediate-mass of of centre existence the the of problem The Context. Abstract: dynamics stellar observations; holes; Keywords: Eprint: Authors: in hole black intermediate-mass Centauri an omega of estimate mass A r xlctygvni em ftesnl-atcecnnclvrals h no- The co- variables. Lorentz imposed. not of canonical is condition variables world-line single-particle position the the variant because apply of not does terms theorem variables interaction in vari- canonical given rest-frame The and explicitly center-of-mass invariance. are and the Lorentz momentum for global linear functions by generating total demanded ous the as between velocity relation center-of-mass the the with accordance vari- rest-frame in and are center-of-mass between ables Hamiltonians post-Newtonian variables. the zero rest-frame in terms and of mixture sec- center-of-mass The counted canonical formal fully are through into spins transformed ones are the order, spinning where order, for post-Newtonian and ond order post-Newtonian third through . 8( + 0 . 9 http://arxiv.org/abs/1002.5037 − ich,P. Miocchi, h eetycntutdHmloin o pnesbnr lc holes black binary spinless for Hamiltonians constructed recently The 1 rq;msiebnre fbakhls otNwointer;spin theory; post-Newtonian holes; black of binaries massive gr-qc; . sr-hG;atohsc;goua lses nemdaems black intermediate-mass clusters; globular astrophysics; astro-ph.GA; 2) × o tr itiueaon asv lc hole black massive a around distribute stars How 10 − 3 ti lofudta h oe ilsafi fteline-of- the of fit a yields model the that found also is It . WNotes GW M BH / M =

39 oe esfrG science GW for News & Notes Notes & News for GW science 40 WNotes GW Eprint: Authors: discs accretion con- in vertical vection to due transport momentum angular the On 0.3) +/- < (3.1 13,000 = range M of estimate mass total eoln lc oe nti a ecnsuyhwtepoete ftesystem, the of properties the how study can we way the this by disc In thus accreting detector", the hole. in "shock produced black a shocks recoiling construct the of to location technique precise new the determining a employ non- and first extended the discs a of perform Keplerian of simulations we merger hydrodynamics specifically, the relativistic More by produced general holes. hole two-dimensional black black the supermassive of of velocity system recoil binary the to and mass of loss Abstract: relativity numerical Keywords: Eprint: Authors: rela- discs general non-Keplerian of holes: simulations black tivistic recoiling of counterparts EM unsta- sufficiently maintained. a be that can provided profile evolution, temperature disc vertical much global ble always explain might convection to is that way transport indicate another results momentum These be angular observations transport. heat the with vertical that compatible the than however conditions, weaker find certain momentum We under angular is, discs. outward that of drive rate can a at convection we transport turbulent methods, spectral strongly momen- high-resolution that angular Using transporting show convection. of thermal possibility a turbulent this the be by undergo revisit tum not we to may letter, appears discs this accretion In instability of instability. magnetorotational regions ionized the poorly Although process, promising debated. been long Abstract: Keywords: http://arxiv.org/abs/1002.4185 http://arxiv.org/abs/1002.4621 eu,G;Oive .I. G. Ogilvie, G.; Lesur, aot,Oid;Rzol,Lcao e an,Lc;Plnul,Carlos Palenzuela, Luca; Zanna, Del Luciano; Rezzolla, Olindo; Zanotti, eivsiaetednmc facrubnr icta epnst the to responds that disc circumbinary a of dynamics the investigate We h ehns faglrmmnu rnpr naceindsshas discs accretion in transport momentum angular of mechanism The crto ic;atop.P sr-hS;atohsc;E counterparts EM astrophysics; astro-ph.SR; astro-ph.EP; discs; accretion sr-hH;E oneprs rq;msiebnre fbakholes; black of binaries massive gr-qc; counterparts; EM astro-ph.HE; M o tr itiueaon asv lc hole black massive a around distribute stars How BH 2)i eurdt ac h ue ufc rgtesprofile. brightness surface outer the match to required is 12’) × 10 6 M

a 1 2010 21, May hsgvn nIB asi the in mass IMBH an giving thus , oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 iaywt oa mass total with binary atro e mle.I ofimdb oespitctdcluain uha binary such of calculations merger sophisticated the of more counterpart by electromagnetic system. confirmed an black-hole to If lead indeed smaller. could few signal a of factor produced a luminosity the above ana- that value relativistic 2009, peak the Corrales a on of reach based evolution can approximation isothermal an the At through of short. show, logue unrealistically we are the time that of times same estimates cooling the account yielding the into thus question taking transfer, here properly radiation we the without accre- computed works, In mass when similar the sources. luminosity in these affect bremsstrahlung from done hole, emission what black electromagnetic with the the on of contrast imprinted velocity are recoil and and rate mass tion spin, the as such eit asBakHl nESO243-49 in Hole Black Mass Inter- the mediate of Observations Follow-up Swift and Chandra Keywords: Eprint: Authors: spins hole black massive of Evolution Keywords: Eprint: Authors: quasars. in holes black of spins discuss the and I for remnants, events. merger implication spins accretion in the hole holes and black mergers black accreting of of massive combination simulations of recent the describe evolution to the due history, here gravi- cosmic impulsive discuss of the the I emission along of anisotropic merger. cause to at be due waves galaxies, km/s, tational hole in thousands black to holes massive up black that recoil", of clear "gravitational retention became energy the it much affect Recently how also determine itself. spins also hole the Spins from quasars. extractable is from output radiative the hence Abstract: holes black vations http://arxiv.org/abs/1002.3827 http://arxiv.org/abs/1002.3625 ootr,Marta Volonteri, eb .A;Bre,D;Gdt . evla,M;Frel .A;Ots .R. S. Oates, A.; S. Farrell, M.; Servillat, O.; Godet, D.; Barret, A.; N. Webb, lc oesisafc h fcec fte"lsia"aceinprocesses, accretion "classical" the of efficiency the affect spins hole Black sr-hC;atop.E srpyis omlg;si;supermassive spin; cosmology; astrophysics; astro-ph.HE; astro-ph.CO; sr-hH;atohsc;IR;itreit-asbakhls obser- holes; black intermediate-mass IMRI; astrophysics; astro-ph.HE; o tr itiueaon asv lc hole black massive a around distribute stars How M ' 10 6 L M '

n ess o eea asa auswihare which values at days several for persist and 10 43 WNotes GW erg / s tabout at ∼ 20d fe h egro a of merger the after

41 oe esfrG science GW for News & Notes Notes & News for GW science 42 WNotes GW bevtosw euetems crto aeo 0 snbakhl ihthe environment. with an such hole with black compatible Msun is 500 this a that show of X-ray and rate latest luminosity the accretion observed Using mass that region. the imply forming deduce star could a we This of near-UV. observations edge the the near than sug- situated and stronger be GALEX may is from HLX-1 emission data elongated far-UV archival is by the supported emission that is UV gests This the HLX-1. that of evidence mag- direction is limiting the 3sigma there in a However, to mag. down we position 20.25 images, Chandra of the uvw2 nitude at Telescope source UV UV/Optical with a field Swift detect the to all failed in Combining sources X-ray catalog. 3 2MASS of bore- the positions a the following cross-matching found by was 0.3" correction of sight error 95% RA=01h10m28.3s conservative of A Resolu- position High source Dec=-46d04’22.3". a the and determine Using we observed. Chandra, luminosities onboard the potentially Camera at tion could hole it black a whether nourish establish nec- and to is form it environment identification, HLX-1’s hole determine black to mass essary intermediate po- the source reinforce improved an further To needs in-turn sition. which investiga- X-rays, follow-up than requires other This wavelengths with affiliation. at HLX-1 its tions confirm of to association As essential the is on holes. it depend 243-49, black estimate ESO mass mass intermediate the thus of and existence luminosity the the for evidence strong provides 49 Abstract: ial,w xmn h eprlcnegneo h vrg tes n hwthat show and stress, resolved. average and the captured of fully convergence be temporal must the corona examine global the we for Finally, of requirement extent convergence vertical new in the a disk – suggest the simulations and of field, regions local different momen- the between magnetic determining angular of corona) vertical importance of low-density of the the strength demonstrate We patches (through the disk. linkages local control the Moreover, of and much across stimulate transport simulations. to tum that local enough manner strong in a are in found stress field field that Maxwell magnetic local to vertical the similar local that is self-generated show We the with viscosity. correlated or is resistivity magnetic explicit net zero no glob- with and disks are flux geometrically-thin studies, model simulations box The shearing robust. ally local the by via driven turbulence discovered for instability, laws magnetorotational scaling whether determine to order in simulations Abstract: holes black sive Keywords: Eprint: Authors: in Turbulence Global Disks Accretion and Local Between Connections http://arxiv.org/abs/1002.3611 oaha aemA;Ryod,CrsohrS;Amtg,Pii J. Philip Armitage, S.; Christopher Reynolds, A.; Kareem Sorathia, eaayeasieo lblmgeoyrdnmc(H)aceindisk accretion (MHD) magnetohydrodynamic global of suite a analyze We h rgts lr-uiosXrysuc L- nteglx S 243- ESO galaxy the in HLX-1 source X-ray Ultra-Luminous brightest The crto ic;atop.E srpyis Mcutrat;supermas- counterparts; EM astrophysics; astro-ph.HE; discs; accretion o tr itiueaon asv lc hole black massive a around distribute stars How

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 h -a oiinsrntesteagmn gis akrudAGN. background at a emission against radio argument detectable the of ongoing strengthens lack position indicate The X-ray could HLX-1. the that around region emission the sub-arcsecond UV in to of formation position detection star X-ray the the report refined also have We We source accuracy. bands. intriguing radio this and on black UV results mass X-ray, multi-wavelength in intermediate latest the of present existence we the Here for holes. evidence strong provides currently 49 Abstract: observations holes; field. magnetic initial time the a of on mixing away turbulent dies with relation consistent flux-stress is local that the scale in drift secular long-term initial an Keywords: Eprint: Louis Authors: Holes Light- Black the Supermassive est Assembling from Signal Wave Gravitational Keywords: Eprint: D. Barret, A.; Authors: Black HLX-1 Mass 243-49 Intermediate ESO Candidate the Hole of Observations Further inlwvs euehg eouincsooia -oysmltost rc the track Inter- to simulations Laser N-body the cosmological gravita- for resolution detect high goals to use science mission We NASA/ESA primary waves. planned the tional a of (LISA), one Antenna is Space observing range ferometer because mass important this particularly is in holes as- SMBHs black The mass stars. lower III these mass Population of solar of sembly remnants million the 10 from of (SMBH) growth holes the black from supermassive signal wave gravitational the calculate We Abstract: holes black supermassive http://arxiv.org/abs/1002.3378 http://arxiv.org/abs/1002.3404 arl,S . evla,M;Ots .R;Hyod . oe,O;Wb,N. Webb, O.; Godet, I.; Heywood, R.; S. Oates, M.; Servillat, A.; S. Farrell, h rgts lr-uiosXrysuc L- nteglx S 243- ESO galaxy the in HLX-1 source X-ray Ultra-Luminous brightest The olyBcemn,Kly ii,Mrsa;Sgrso,Sen;Rubbo, Steinn; Sigurdsson, Miroslav; Micic, Kelly; Holley-Bockelmann, sr-hC;atop.E srpyis MI nemdaems black intermediate-mass IMRI; astrophysics; astro-ph.HE; astro-ph.CO; sr-hC;atohsc;csooy asv iaiso lc holes; black of binaries massive cosmology; astrophysics; astro-ph.CO; o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW

43 oe esfrG science GW for News & Notes Notes & News for GW science 44 WNotes GW bevdeet vr1 er,atog h cuayo hsrt safce ycos- by affected is rate this of accuracy during 500 the variance. roughly Group although mic yields Local years, universe the 10 the over of like events volume volume observed the a over signal- extrapolated within a – the occur with assembly of sources 30 SMBH model 40 than about accurate pre- greater yields an on estimate ratio as best depends well to-noise our source as scale; LISA galaxy hole new a black ra- this on the dynamics mass of onto extreme rate accretion event or gas the mergers for that scriptions SMBH find for We likely gravi- used will the inspirals. is signal tio in than this considered technique of widely different characterization been a and require not detection has community; merger ratio wave mass tational high of type This redshifts at SMBHs and volume 2. our holes than from black less band mass LISA intermediate the between in mergers source of common SMBHs consists and most accretion, the the gas of that friction, growth find We dynamical the feedback. combines model that and approach halos, semi-analytic matter a dark with host the of history merger Authors: black binary precessing of holes merger the from spins Final X-ray indices. and spectral NIR observed between the in model differences the the cool in explain electrons break can that spectral NIR-emitting wavelengths a very the produces cool while electrons This timescale emitting slowly. X-ray dynamical more the typical Gauss the 5-30 about on emis- of quickly X-ray field the magnetic for a explanation In feasible "cooling sion. more a a Instead, provides A*. model Sgr synchrotron for mecha- Trying break" unrealistic Compton are inverse that date. through parameters to flare physical implies this X-rays nisms of and characteristics spectral (near)-infrared the in explain simultaneously to observed be to flare Abstract: Keywords: Eprint: O. F.; Pfuhl, Eisenhauer, K.; H.; T. Bartko, Fritz, S.; T.; Trippe, F.; Ott, Yusef-Zadeh, A.; Goldwurm, R.; Genzel, N.; mechanism Authors: emission their and A* Sgr from Flares http://arxiv.org/abs/1002.2885 edn ihe;Sehk,Urc;Bri Emanuele Berti, Ulrich; Sperhake, Michael; Kesden, od-dn . oqe,D;Ta,G;Qaar,E;Glesn . Grosso, S.; Gillessen, E.; Quataert, G.; Trap, D.; Porquet, K.; Dodds-Eden, esmaiercn bevtosadmdln ftebihetSrA* Sgr brightest the of modeling and observations recent summarize We sr-hG;atop.E srpyis bevtos aitru A* Sagittarius observations; astrophysics; astro-ph.HE; astro-ph.GA; o tr itiueaon asv lc hole black massive a around distribute stars How

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 Abstract: holes black the in degrees config- 20 binary separated about widely from and resulting urations. magnitude, spin lim- final spin accuracy the dimensionless intrinsic predicting in an the direction induces in precession 0.03 that black of out stellar-mass itation point in also and We redshifts high binaries. at hole mergers spin hole significant black produce massive could in they alignment and binaries, effects Resonant comparable-mass the for spin. stronger final if angu- are average orbital other the the each (decreasing) to increasing with respect thus spins momentum, with lar (anti-aligned) hole aligned black partially binary initially the were reso- spins M, (anti-align) Spin-orbit align 10 inspiral. to = post-Newtonian tend the r nances momentum during at angular distorted isotropic orbital significantly the remain be with can M aligned partially =1000 initially begin. r are that typically at distributions simulations distributions numerical-relativity spin where isotropic M orientations Although 10 spin exam- near of We r distribution the separations motion. affects at evolution of post-Newtonian equations these this post-Newtonian between how by evolution ine described binary Fortunately, well M. is 10 separations r separations binary at reaction Abstract: spin theory; post-Newtonian Keywords: Eprint: Keywords: Authors: Galac- Center the Searching tic within – populations stellar Center young Galactic missing the the of Survey Palpha HST Eprint: C. Lang, G.; Schneider, A.; E. Mills, J.; e g) hc astecnrl0.65 central the maps which (gc), ter ihnls asv trcutr/rus oprdt h he asv ns Our ones. massive are three they the that to suggests compared Pa sources clusters/groups, field star these massive near of clusters less distribution star within massive spatial young loosely three The of outside A*. located Sgr are compared them of gc, Half the stars. within sive Pa stars 157 massive find We of observations. inventory previous complete to more a with us vides α oacntol eovspeiul elkonlresaefiaet nofine into filaments large-scale well-known previously resolves only not mosaic http://arxiv.org/abs/1002.2643 http://arxiv.org/abs/1002.2611 epeetpeiiayrslso u S Pa HST our of results preliminary present We og . ag .D;Ctr,A;Sooy . ors .R;Mauerhan, R.; M. Morris, S.; Stolovy, A.; Cotera, D.; Q. Wang, H.; Dong, h nprlo iaybakhlsi oendb rvttoa radiation gravitational by governed is holes black binary of inspiral The sr-hG;g-c asv iaiso lc oe;nmrclrelativity; numerical holes; black of binaries massive gr-qc; astro-ph.GA; sr-hG;atohsc;osrain;SgtaisA;supermassive A*; Sagittarius observations; astrophysics; astro-ph.GA; o tr itiueaon asv lc hole black massive a around distribute stars How × .5dgesaon g * hssre pro- survey This A*. Sgr around degrees 0.25 WNotes GW α mtigsucs hc r vle mas- evolved are which sources, emitting α uvyo h aatcCen- Galactic the of survey

45 oe esfrG science GW for News & Notes Notes & News for GW science 46 WNotes GW Irgos npriua,w n w ein ihlresaePa large-scale with Pa H regions of and two shocks tens find bow and we as particular, such In objects, regions. extended new II many reveals also but structures, Eprint: metric-less Authors: banks and template stochastic metric-guided and random the of in placement issues art: Cover masses hole black the feedback of constraints. their and phenomenological and the dispersions to mass velocity near The initial the are it. of their destroy values to according able final way never the is different efficiency, in it in has but mass bar grow hole the holes of black bar, ellipticity black central stellar the The on A simulations. effect our mild scenario. a all cosmological general in fully present a and is in with Gyrs, disk (disk 10 comparison stellar lasting same a the for make same hole) We the black center. of without its one sur- in the hole the with black simulations on these without feedback use of disk energy We results the different compare bar. and We the masses gas. rounding of initial growth harboring different systems the with mass on holes disk-to-halo out hole black isolated point same to black the is massive paper of central this simulations of a N-body-SPH aim such The formation of present. star is impact hole the the the black where central analyzing disks, a of stellar-gaseous and triggered, aim inside is instability the bar with the performed of simulation growth numerical present we paper Abstract: holes black sive Keywords: Eprint: super Authors: harboring disks holes of black massive instabilities and Evolution . gc the in ago star Myr of 350 episode about an process suggest formation histories formation star 1.90 different with in tracks distribution evolutionary magnitude in the Furthermore, of previously. Comparisons known not detect we were survey, which our activities, formation star cent http://arxiv.org/abs/0909.0563 http://arxiv.org/abs/1002.2562 ac,Ga ai;Vlinr,Michele Vallisneri, Mario; Gian Manca, Giuseppe Murante, Valentina; Romeri, de Anna; Curir, h a omto ssila pnpolmi oenatohsc.I this In astrophysics. modern in problem open an still is formation bar The crto ic;atop.O srpyis Mcutrat;supermas- counterparts; EM astrophysics; astro-ph.CO; discs; accretion α mtigsucsi h eaieGlci ogtd ugsigre- suggesting longitude Galactic negative the in sources emitting o tr itiueaon asv lc hole black massive a around distribute stars How ∼ . ilo tr,ms fwihaerdgat rABstars. AGB or giants red are which of most stars, million 0.6 a 1 2010 21, May µ n hs rmtestellar the from those and m

ifs emission diffuse oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 hieo ceeadisipeetto eal ilsilne ob fine-tuned be to need still will details implementation problem. each its for placement and separately specific randomized the scheme that of a but problems, class of search broad choice many to the answer that promising a argue represen- offers We triangulation-based algorithms discrete geometry. a local with we replaced of Specifically, be tation obtain. can to metric difficult be the the may how without which show and metric, with signal Riemannian manifolds a signal of curved use im- in the algorithms important, these most sequences; of number plementation avoiding) (self quasi-random boundaries; per- of parameter-space of use and effects the size the the banks; explore template we placement: resulting the article randomized of this in formance In issues practical others. by and to theoretical close placement several too random are enhances that ran- templates which as rejecting such placement, selectively yet strategies stochastic placement flexible, and randomized general, placement in a dom found that models be suggested can signal have alternative simple authors efficient Various beyond regular generalize parameters. on few to with based difficult algorithms are placement meshes current parameter-space the Unfortunately, sources. gravitational- modeled wave of searches matched-filtering exhaustive for requisite crucial Abstract: algorithms search estimation; parameter methods; numerical MLDC; Hastings; Keywords: eosrt httewr oeb h isptv opnn ftecomputed the of component dissipative we the code our by of done test work a the as energy that radiation; orbital gravitational demonstrate of time-domain through loss a the momentum for in angular responsible pieces and is two and component these piece, dissipative disentangling conservative The for a framework. method as simple well as a piece describe dissipative we a regularization. contains mode-sum self-force dimensions). via total 1+1 obtained then The (in is domain orbit the time along the self-force physical in The for evolution solve numerical and using harmonics, tensorial harmonic For equa- into each perturbation particle) a gauge: metric delta-function Lorenz around the Lorenz-gauge the by the orbit (sourced in decompose tions geodesic out we (bound) orbit, carried geodesic is generic given calculation a a The in hole. particle black pointlike Schwarzschild a on acting force Abstract: Keywords: Eprint: Authors: orbit eccentric hole black in Schwarzschild particle a around a on self-force Gravitational http://arxiv.org/abs/1002.2386 aak er ao Norichika Sago, Leor; Barack, h fcetpaeeto inltmltsi oreprmtrsaei a is space source-parameter in templates signal of placement efficient The epeetanmrclcd o acltn h oa rvttoa self- gravitational local the calculating for code numerical a present We aaaayi;dtcos rq;isrmns nefrmtr;Metropolis- interferometers; instruments; gr-qc; detectors; analysis; data MI edscmto;g-c ueia ehd;sl force self methods; numerical gr-qc; motion; geodesic EMRI; o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW

47 oe esfrG science GW for News & Notes Notes & News for GW science 48 WNotes GW hsaayi,addsusftr applications. future discuss and conserv- the analysis, in to this shift due Lett. the a Rev. orbit of circular As [Phys. stable value self-force innermost the orbits. ative the reported strong-field of recently frequency eccentric and we in location code time the our first of phases; the application orbital for concrete the here first of calculated evolution energy is of the piece rate influences time-averaged this it the but affect loss, not angular-momentum does force and self The the solutions. of numerical momen- wave-zone piece angular the conservative and from energy independently of extract fluxes we which asymptotic tum, the by balanced precisely is force bevr,terss n opttoa srpyiit,w lorve h cross- the review also we by terminology. readable astrophysicists, disciplinary observations review computational in this make art and to the theorists, order of In observers, state systems. the these discuss of clus- and modeling star beyond, dynamical massive and and young Group known Local currently the the in of ters properties global the focus describe than We we massive review more this In and than cousins, old, exotica. younger older stellar clusters their in such star few rich although on a unusually clusters, only are massive far clusters, young So globular in the binaries. found and unusual stars been many exotic have for of nurseries objects range the wide be a to including they expected popu- objects, are and cluster clusters young function, massive of Young mass mechanisms star-cluster formation lations. the the on unresolved study constraints distant to excellent The used provide effectively ecological dynamics. be the stellar re- may and and function to clusters mass evolution enough stellar stellar close the between are studying and for interplay that starburst interest clusters in prime massive of abundant young are particularly solve few are The Way they Milky but galaxies. the Group, interacting in Local exist the examples and Several Galaxy galaxies. of blocks building fundamental Abstract: dynamics stellar holes; black intermediate-mass IMRI; hw; Keywords: Eprint: Authors: clusters star massive Young http://arxiv.org/abs/1002.1961 wr,SmnPreis ciln tv;Gee,Mark Gieles, Steve; McMillan, Portegies; Simon Zwart, on asv lsesaedneageae fyugsasta omthe form that stars young of aggregates dense are clusters massive Young sr-hG;atop.R srpyis lblrcutr;GU GRAPE GPU; clusters; globular astrophysics; astro-ph.SR; astro-ph.GA; o tr itiueaon asv lc hole black massive a around distribute stars How ∼ ∼ 10 102 100 4 M 911(09] eew rvd uldtisof details full provide we Here (2009)]. 191101 ,

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a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 h asrto fterhs egn aais u r osqec ftecomplex the of dynamics. consequence merger a are and trace but accretion necessarily galaxies, between not merging interplay do findings host nuclei These their galactic of in ratios. ratios pairs mass mass MBH the major minor of with ratios that mass pairs suggesting the 1:2, MBH that as to indicate large rise as final give be the can encounter, can mergers the pairs galaxy of MBH geometry resulting the the initial and of larger disks the ratios with galactic on mass the pairs Depending in MBH promptly. gas that cold and so of effectively fraction itself, more pair produced remnants the the are of of ratios nuclei ratio mass the mass in final MBHs. formation the the pair of with MBH ratio of correlates mass efficiency 1:10 the initial that find the en- also of of We increase episodes an distinct cause undergoes which MBH accretion the companion hanced inside the circularization galaxy, orbital primary and the host of its disk on acting torques tidal strong to Owing of Mergers Galaxies Minor Disk in Pairs Hole Black Massive Growing ihtelresaesrcueo h aayo ihec te.Teaceiggas accreting The other. each with correlation or no galaxy have the flows of gas structure whose large–scale occur events, to chaotic the appears small–scale, with Accretion very of nuclei. series galactic a active in in outflow and accretion review I Abstract: holes black permassive Keywords: Eprint: Authors: Galaxies Active in Outflow and Accretion red- a at formation pair 1:10 MBH consider We of peak processes. of predicted both shift a from around feedback ac- occurring as and events formation well merger star as includes MBHs, set during the simulation pairs onto Our (MBH) cretion galaxies. hole disk black of massive mergers of minor evolution the investigate to simulations Abstract: Keywords: Eprint: J. Wadsley, T.; Authors: z http://arxiv.org/abs/1002.1808 http://arxiv.org/abs/1002.1712 ∼ ig Andrew King, algr,S;Kznzds . ae,L;Cli . elvr,J . Quinn, M.; J. Bellovary, M.; Colpi, L.; Mayer, S.; Kazantzidis, S.; Callegari, epromasieo ihrslto mohdpril hydrodynamics particle smoothed high-resolution of suite a perform We 3 sr-hC;atohsc;csooy asv iaiso lc holes black of binaries massive cosmology; astrophysics; astro-ph.CO; crto ic;atop.O sr-hH;E oneprs pn su- spin; counterparts; EM astro-ph.HE; astro-ph.CO; discs; accretion ntesniiiywno fteLsrItreoee pc Antenna. Space Interferometer Laser the of window sensitivity the in , o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW

49 oe esfrG science GW for News & Notes Notes & News for GW science 50 WNotes GW rcin a rdc aaywd uflw,icuigfsi uflw ngalaxies in activity. AGN outflows current fossil little is including gas there small outflows, where far with galaxy-wide a events produce accretion imply Minor can would observed. fractions not outflow actually did (‘energy-driven’) than gas mass resulting shocked SMBH the the smaller If above, prevented. asserted is as growth hole cool black further reached, is mass oe eoiis h hl fmte wp pb h hce idsal nesthe unless stalls value wind the shocked reached the has by mass up hole swept black matter of shell The with velocities. associated in lines lower observable the emission be lower–excitation with may and region interacts continuum Compton cooling it inverse this as an and galaxy, shock host cooling the strong of medium a and interstellar creates helium– wind of The lines resonance iron. of hydrogenlike presence the implying parameters ionization and iebakhlst rw hwta hypouewnswt velocities with winds produce they that show supermas- I the for grow. order to in holes common black be sive must AGN in driver. episodes underlying accretion the be Eddington may which merger, galaxy a in involved small gas a the only represents of probably fraction and momentum angular specific low extremely has nuprlmt hsptnilypoie aubenwisgtit h rcse of processes evolution. the and into formation insight SMBH new defines and valuable relation provides galaxy M-Sigma potentially This observed limit. the upper implies an available also of r. it result resolving However, a of be simply resolution. basis may spatial the relation on M-Sigma observed solely the M-Sigma justified shows be Letter an This fu- not Consequently, produce should se- estimates SMBHs values. and M observed random proposed M with ture These random consistent a beta=4.0, resolved. given alpha=8.3, of are spatially relation Mpc, is 100 r than when closer galaxies All lected Sigma, relation. of M-Sigma the values follow known pop- not a do with to that argument SMBHs r further and the for galaxies applying of of galaxies ulation effects res- additional the spatial quantifies pre-select uses Letter and This argument estimates studies. (r) SMBH M influence" interest of some great "sphere exclude be The to to catalog. olution continues M there the evolution, to adding and models in formation + for SMBH alpha implications = and important log(M) galaxy has by of relation described this is As (Sigma) km/s). dispersion beta*log(Sigma/200 velocity stellar bulge and (M) Abstract: holes black permassive Keywords: Eprint: Influ- Authors: of Sphere from Arguments ence Derived Relation M-Sigma The http://arxiv.org/abs/1002.1705 acedr D. Batcheldor, h bevdrlto ewe uemsiebakhl SB)mass (SMBH) hole black supermassive between relation observed The sr-hC;atop.A srpyis omlg;osrain;su- observations; cosmology; astrophysics; astro-ph.GA; astro-ph.CO; o tr itiueaon asv lc hole black massive a around distribute stars How M σ mle ythe by implied a 1 2010 21, May M − σ eain nethis Once relation. v ∼

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1 c oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 omlg u eainhsbe oprdwt h rdcin ftoglx for- galaxy two Simulation. Millennium of the predictions on the based with models compared LambdaCDM mation the been ex- of has samples framework relation three the our In using cosmology by galaxies. confirmed of catalogues been different has from statement tracted this of validity The laws. eew ics t ehns n h mlctosfrteGlci ete home Centre, Galactic disc. the stellar circum-MBH for one implications least the at cluster. and eccentricities to stellar mechanism lower surrounding its or the discuss or of higher we high distribution Here attain density very to the either stars on achieving significantly for (MBHs) depends preference stars holes The in black results eccentricities. massive which low orbiting clusters, stars stellar of in discs embedded eccentric coherently in occurs Abstract: Keywords: Eprint: Back- Authors: on Dependency Cluster Stellar Instability: ground Disc Eccentric The corre- galaxies. the the for than better diagram of data age-temperature motions experimental the an random fits as relation of This reinterpreted energy be kinetic can the bulges and sponding galaxies host the of center Abstract: holes black permassive Keywords: Eprint: Authors: models numerical and data real between versus mass SMBH The Authors: Centre Galactic the in Segregation Mass http://arxiv.org/abs/1002.1277 http://arxiv.org/abs/1002.1703 aia,Ann-Marie Madigan, den van S. Bergh, F.; Marulli, L.; Mancini, A.; Feoli, omn lvs aia,Ann-Marie Madigan, Clovis; Hopman, nti ae ervstte"ceti icisaiiy,a ntblt which instability an instability", disc "eccentric the revisit we paper this In h eainbtentems fsprasv lc oe oae nthe in located holes black supermassive of mass the between relation The sr-hG;atohsc;Nbd;SgtaisA;selrdynamics stellar A*; Sagittarius N-body; astrophysics; astro-ph.GA; sr-hC;atop.A srpyis omlg;osrain;su- observations; cosmology; astrophysics; astro-ph.GA; astro-ph.CO; o tr itiueaon asv lc hole black massive a around distribute stars How M WNotes GW G σ 2 eain comparison A relation: M bh − M G , M bh − L G and , M bh − σ

51 oe esfrG science GW for News & Notes Notes & News for GW science 52 WNotes GW iei h aatccnr G)is in (GC) centre reached Galactic is the state in time steady cal- Fokker-Planck that of show use and the with culations, mass-segregation driving physics the however, discuss obtained. We massive are and distributions rare steeper are much and stars down heavy breaks steeper the limit with If zero-ﬂow reached, stars. the are massive 3/2

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a htdvre to- diverges that oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 nteasneo srpyia oerud,LS ol eetsgaswt energy with that, signals show detect We as could low LISA as detectors. foregrounds, densities astrophysical length of arm absence combination unequal the new for in a insensitivity derive partic- this and from interferometry, maintains delay formed that time channels" the "null of insensitive combinations dis- wave We ular gravitational contributions. of noise instrument role and the gravitational cuss the apart tease to used be ihOdrPs-etna i fteGravitational Geom- etry Schwarzschild the the in Orbits of Circular for Self-Force Fit Post-Newtonian High-Order Abstract: Keywords: Eprint: Authors: A* Sgr of Models Numerical Keywords: Eprint: Authors: rather suggest models Our ( models. spin numerical hole con- the black Monte modeling of high of image space combination GHz parameter The 230 the and GHz. strains calculations 230 distribution recon- around to energy slope models spectral spectral our Carlo the scale and spins, We flux hole inclinations. black the and various struct ratios, for temperature models sur- electron flow parameter to the a of perform ion We properties GHz. radiative 230 compare study at and and observations A* gamma-rays) VLBI vey Sgr the of to to images image millimeter model of also (from radiative size we the band scheme relativistic tracing broad general ray a a use Using We produce spectrum. to A*. and Sgr methods in transfer accretion of simulations dynamic ( the from data Challenges. Data simulated LISA using background, Mock approach of wave this round gravitational third of stochastic effectiveness assign a the and of demonstrate characterize detection and for, search the to for able levels is confidence that pipeline analysis Bayesian to-end T i / T e ∼ http://arxiv.org/abs/1002.1261 http://arxiv.org/abs/1002.0726 3 ocboza . ame .F;Dlne . hoaa . en,P K. P. Leung, H.; Shiokawa, J.; Dolence, F.; C. Gammie, M.; Moscibrodzka, lnht u;Dtelr tvn ic lxnr e htn,BradF. Bernard Whiting, Le; Alexandre Tiec, Steven; Detweiler, Luc; Blanchet, n ihiciainage ( angles inclination high and ) erve eut rmgnrlrltvsi xsmercmagnetohydro- axisymmetric relativistic general from results review We sr-hH;osrain;SgtaisA;spin A*; Sagittarius observations; astro-ph.HE; eea eaiiy rq;ps-etna hoy efforce self theory; post-Newtonian gr-qc; relativity; general o tr itiueaon asv lc hole black massive a around distribute stars How Ω gw a ∗ = ≈ 6 0 × . 9 10 ,eeto eprtrscoet h o temperature ion the to close temperatures electron ), − 13 ihjs n ot fdt.W eciea end- an describe We data. of month one just with WNotes GW i ≈ 0deg 90 ).

53 oe esfrG science GW for News & Notes Notes & News for GW science 54 WNotes GW ae eeto fgaiainlwvsb ntuet uha IOadVirgo. and LIGO as such instruments by waves ground- the gravitational quantitative for of a waveforms detection in inspiral based results complete generate numerical work to combine as Our that so efforts framework LISA. analytical on instrument impact wave an gravitational have space-based also will the inspirals ratio by high mass analysed with extreme efforts of be confirm SF waveforms and to also template PN of we between synthesis fit interplay the for This best important higher coefficient. our is 3PN of In the estimates of level. value give 7PN the to precision the able to are up we contributions particular Furthermore order a in used observable. coefficients are non-logarithmic and invariant 5PN ratio, gauge and mass 4PN the the in measure order support accurately first results to through dy- SF calculations perturbative the PN numerical of analytic The part the system. well conservative binary 4PN the compact leading in a the terms of namics analytically logarithmic 5PN compute PN order next-to-leading we higher the theory obtain and PN to standard used helps be Using parameters to data PN coefficients. numerical appropriate the determined allowing in analytically data tremendously SF knowing numerical approximations. that PN the find high that We extremely show to We corresponding information background. physical Schwarzschild contain cir- of a analysis in (SF) orbits self-force cular gravitational the and approximation (PN) Newtonian Abstract: fteANo h urudn oie a.Uigdt rmSNOIa h ESO the at is SINFONI mass from hole data black Using best-fit effects gas. the the Telescope, ionised Large identify surrounding Very to the key on the AGN is the spectroscopy of field that integral concludes assisted and measurements optics and mass adaptive techniques hole gas black observing both that of in field from studies advancement the A recent the drive Centaurus instrumentation how the in shows of mass It overview hole kinematics. an black stellar give the and to measure is to review dedicated supermassive this been the feedback have of of aim and mass The the feeding the of the hole. on determination black understand influence accurate and an its needs model and To one hole mechanisms black detail. supermassive great the in study environment to example prime the Abstract: holes black Keywords: Eprint: Authors: Kinematics Stellar and Gas- Centaurus by of Revealed Heart A: the at Hole Black Supermassive The (from ohwt im ros.Ti soeo h laetgsv trcmaio of comparison star vs gas cleanest the of one is This errors). sigma 3 with both H http://arxiv.org/abs/1002.0965 2 emyr Nadine Neumayer, ieais and kinematics) tls hn4Mcdsac h ai aayNC52 CnarsA is A) (Centaurus 5128 NGC galaxy radio the distance Mpc 4 than less At ecniu rvoswr ntecmaio ewe h post- the between comparison the on work previous a continue We sr-hC;atop.M srpyis bevtos supermassive observations; astrophysics; astro-ph.IM; astro-ph.CO; o tr itiueaon asv lc hole black massive a around distribute stars How M BH = (5 . 5 + / − 3 . 0) a 1 2010 21, May × 10 M 7 BH M

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oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 relation. a Abstract: Keywords: drag-free LISA Authors: the on Dust Constellation Interplanetary of Effects Abstract: ics Keywords: Eprint: Authors: poten- perturbed a tial in evolution dynamical – disc Stellar Eprint: Mauro Sereno, Antonello; Ortolan, Giulio; Mazzolo, Francesco; Marzari, Philippe; been the have with that interaction stars gravitational as the explained to are due birth outliers disc. given structure The circum-nuclear have gaseous parent GC. may the the disc from in stellar stripped stars thin young present single initial We all complicated a clouds. to rather that gas interacting in showing and lies solution infalling solution alternative two disc- possible least the at One of to assuming any GC. fails to conditions, belong the it not in do but self- evidently structures thin orbits, that stars like a rotating of in coherently tens several formation on of star origin stars explain the forms of naturally scenario disc promissing gravitating most The problems. ious h eitosfo h IAkpeinobt rudteSn hsaayi can analysis This Sun. the around get orbits to keplerian equations LISA planetary Gauss the the from the integrated deviations fit perturbing we that the The gravitational Then distributions density the light. ID trajectories. account zodiacal some spacecraft for observed into calculated the take been on has we field (ID) particular, gravitational orbits Dust In free-fall Interplanetary the estimate of mission. accurately effects space to LISA crucial is the System of Solar the in fields tional M BH eemnto,adbig etuu noareetwt the with agreement into A Centaurus brings and determination, http://arxiv.org/abs/1002.0489 http://arxiv.org/abs/1002.0718 ur Ladislav Subr, h nlsso o-aitv ore fsai rtm-eedn gravita- time-dependent or static of sources non-radiative of analysis The oeso h rgno on tr nteGlci eteaefcn var- facing are Centre Galactic the in stars young of origin the of Models edno asm;D aci arzo ePer,Rbro Jetzer, Roberto; Pietri, De Fabrizio; Marchi, De Massimo; Cerdonio, eetr;g-c ntuet;interferometers instruments; gr-qc; detectors; sr-hG;atohsc;osrain;SgtaisA;selrdynam- stellar A*; Sagittarius observations; astrophysics; astro-ph.GA; o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW M BH − σ

55 oe esfrG science GW for News & Notes Notes & News for GW science 56 WNotes GW Eprint: Center Galactic Authors: the in Collisions Stellar of Impact The densities. LDM and ID on limits during upper collected provide data could Doppler mission the LISA frequency, whole assumptions low strong the very some at ex- Under noise are distributions. displacement LDM fields the and gravitational on ID as for (LDM), similar be Matter to Dark pected Local to extended eventually be rgnlse asdsrbto.Cneunl,tepoete fMH nnearby in MBHs of the of properties ‘memory’ the some Consequently, retain result, Universe a distribution. local as mass the and seed in history, original observed merger dwarfs quiet that the a expect in undergo exist we galaxies also should Dwarf MBHs progenitor universe. of population present leftover a that expect to ural Abstract: holes black Keywords: Eprint: satellites Authors: Way Milky in lurking holes black Massive implica- hole. have black turn supermassive central in the may of This growth IMF. it and regular formation case, black a the stellar-mass the for from of is tions expected population this be larger If would much popu- than observations. a red-giant holes matching contains the center pc way, galactic 0.4 this the to In implies out giants. depleted stars red be main-sequence into could the lation evolution destroy their to prevent likely thus are and encounters and Such stars main-sequence between remnants. those neutron then compact and are dwarfs collisions white common holes, most popu- black The stellar (ie stars). the remnants IMF, compact flatter depleted by much be dominated a may is For in lation holes. closer black much stellar-mass giants red with brighter collisions remove although via to pc unable 0.4 are low-mass to case, out collisions former giants and the red population, In IMF. the flatter differ- dominate much two a stars with 2) main-sequence population and stellar Miller-Scalo the the model 1) We IMFs: center. ent galactic the in giants red of Abstract: Keywords: http://arxiv.org/abs/1001.5451 http://arxiv.org/abs/1002.0338 ais .B;Cuc,R . ameg . zk,S;Dl,J;Fetg M. Freitag, J.; Dale, S.; Nzoke, D.; Malmberg, P.; R. Church, B.; M. Davies, a asnoe . ootr,M;Wle,M . ar .R. J. Gair, G.; M. Walker, M.; Volonteri, S.; Wassenhove, Van ecnie hte tla olsoscnepanteosre depletion observed the explain can collisions stellar whether consider We smsiebakhls(Bs rwfo oe-asses ti nat- is it seeds, lower-mass from grow (MBHs) holes black massive As sr-hC;atop.E srpyis omlg;msiebnre of binaries massive cosmology; astrophysics; astro-ph.HE; astro-ph.CO; sr-hG;atohsc;SgtaisA;selrdynamics stellar A*; Sagittarius astrophysics; astro-ph.GA; o tr itiueaon asv lc hole black massive a around distribute stars How

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 aayszs ncnrs,Pplto I ennshv ihrBO,bttheir but BHOF, dwarf detection. higher their observed a inhibiting for have formation, since cent remnants much per III grown than not Population have less contrast, masses to In decreases is BHOF and sizes. typical cent galaxy their per seeds’ but 40 ‘massive identification, as their below generated favour always MBHs would frac- that occupation z=0. hole masses at black large population the have indication satellite derive clear We the a of were. providing (BHOF) seeds thus the tion mass, of that properties original find the the We what retain of satellites. MBHs compute these part We in most hosted the layers. population for mass MBH the outer of their the properties stripping how different consideration satellites, into dynamically the taking We system, modifies hosts. central interaction rarer the with in seeds’ merging form ‘Massive halos but all remnants, evolve model. PopIII seed than remnant gas- masses via III larger con- formed have Population We seeds’ a ‘massive and today. instabilities to mechanisms: dynamical high-redshift formation different from MBH evolve halo plausible we Way two galaxies, Milky formation. sider dwarf a in MBH MBHs within of of populations efficiency properties MBH the the examine of to indicators order clean In provide may galaxies dwarf eeal ntecr.O h te ad est upcudb rsn nthe preferred. clearly in is present model no be time, interac- could present of the result cusp At a density be objects. could a these giants with hand, bright tions of other deficit the the remnants and On stellar populations, and unobserved stars core. fainter dis- the of article distribution in the This generally distri- reflects the giants that core. old and age." the pc unrelaxed, old of is 0.5 of bution nucleus a the "conundrum that this is is explain interpretation there might straightforward cusp, models A supermas- dynamical density a of a around sorts of what population cusses Instead relaxed a hole. for black expected sive than different very is Way Abstract: holes black supermassive Keywords: Eprint: Authors: Center Galactic the of Models Dynamical Authors: Hole Black Kerr a from Relativistic Jets Launching for Model Connection Magnetic http://arxiv.org/abs/1001.5435 ert,David Merritt, ua,Ioana Dutan, h itiuino aetp od tr nteinrpre fteMilky the of parsec inner the in stars (old) late-type of distribution The sr-hC;atop.A srpyis bevtos tla dynamics; stellar observations; astrophysics; astro-ph.GA; astro-ph.CO; o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW

57 oe esfrG science GW for News & Notes Notes & News for GW science 58 WNotes GW G ieiewe h G uptpwri rvddb h Blandford–Znajek the by provided is power output maximum the mechanism. AGN of the estimation when the with lifetime consistent AGN is result than This longer power. much spin-down be BH can lifetime AGN maximum the tion, by on up depends spin ( parameter on (i) BH torque the can counter-acting of it state magnetic stationary concerned, the a is to that BH found due We the down BH. as the spin far (ii) As and matter particles jets. accreting disc the the angu- by form away The carried ultimately ergosphere. is BH that disc the accretion of the inside from region removed the momentum from lar launched are jets the that so asaceinrt slre than larger is rate accretion mass parameter spin a mo- with angular BHs the consider and We jets, the jets. of the power calculate by launching to transported the laws jets, mentum conservation the relativistic into general rate is the flow jet mass use is We the the energy jet. disc cases the the both launch as In disc, to accretion used dominates. thin and (geometrically) power low-luminosity, dominates, spin-down a power by BH accretion driven when when phase phase first second a a (i) to recurring(ii) undergo with: BH may activity in- BH the its is the energy connects of that assume disc episodes We which available energy. rotational lines the way, BH field the this by In magnetic creased connection). closed trans- the magnetic is by (BH-disc BH converting disc disc the by the of inner energy (BH) the rotational hole the to when black energy, ferred jet Kerr into accreting energy an disc accretion from (AGN) nuclei galactic Abstract: holes black permassive Keywords: Eprint: togeiec o h ako tla upadasmlrt ftelt yelumi- type late the of similarity a and KLF. cusp bulge the stellar find to a We function of nosity distributions. lack energy the spectral for band evidence narrow strong optics adaptive on based Way Abstract: Keywords: Eprint: Authors: cluster star center galactic the of Composition http://arxiv.org/abs/1001.5381 http://arxiv.org/abs/1001.5434 uhoz .M;Shee,R;Ekr,A. Eckart, R.; Schoedel, M.; R. Buchholz, epeetapplto nlsso h ula tla lse fteMilky the of cluster stellar nuclear the of analysis population a present We epeeta lentv oe o anhn eaiitcjt nactive in jets relativistic launching for model alternative an present We sr-hG;atohsc;osrain;SgtaisA* Sagittarius observations; astrophysics; astro-ph.GA; crto ic;atop.E srpyis Mcutrat;si;su- spin; counterparts; EM astrophysics; astro-ph.HE; discs; accretion o tr itiueaon asv lc hole black massive a around distribute stars How m ˙ en esbtcoet .92(hresmdl.I addi- In model). (Thorne’s 0.9982 to close but less being m ˙ ∼ 0 . 001 h aiu au fteB spin BH the of value maximum The . a 1 2010 21, May a ∗ = os)cnb ece fthe if reached be can const) ∼ 10 7 rwe sn the using when yr a ∗ > 0

. 95

, oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 h erhfrsinn lc oebnre nmock in binaries algorithm hole genetic a black using data spinning LISA for search The Abstract: Keywords: Eprint: Authors: in Simulations Relativity Hole Numerical Black Binary of Status Current The Keywords: Eprint: Authors: fteBakHls ehv on ag ubro ieysprtdmdsi the in modes values. separated likelihood widely maximum of similar number large with spins a space found two parameter have and we momentum in Holes, angular loca- Black present orbital sky the the and sources of for ratio ﬁve As mass accuracy. mass, all reasonable chirp with found time, tion not coalescence have the if We recovered comparable, and is 3.2 algorithms. method MLDC LISA existing this mock already of of performance to round the The third better, and the 3.2). from signal (MLDC data the challenge the data of analyze properties to function the response utilizes extended detector which an introduce We algorithm case. genetic non-spinning the multimodal or- to surface and compared likelihood as the spin structure make The in and richer waveform band. the LISA in the complexity bring in precessions sources bital wave gravitational important most the Abstract: holes black supermassive spin; algorithms; search estimation; ltos n mrvmnst h ehd sdt vleadaayebnr black binary the analyse including and evolve ﬁeld, spacetimes. to hole the used methods sim- of the from state to obtained improvements the results and physical of ulations, recent summary codes, short relativity numerical has a of progress here capabilities much present relativity, numerical I in made. problem hole been black binary the of lutions http://arxiv.org/abs/1001.5161 http://arxiv.org/abs/1001.5380 idr Ian Hinder, Farhan Feroz, Stanislav; Babak, Yu; Shang, Antoine; Petiteau, ic h ratruh n20 hc aeldt ogtr tbeso- stable term long to led have which 2005 in breakthroughs the Since olsigmsieBakHl iaisaetesrnetadprobably and strongest the are binaries Hole Black massive Coalescing rq;msiebnre fbakhls ueia relativity numerical holes; black of binaries massive gr-qc; aaaayi;g-c asv iaiso lc oe;MD;parameter MLDC; holes; black of binaries massive gr-qc; analysis; data o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW

59 oe esfrG science GW for News & Notes Notes & News for GW science 60 WNotes GW rvt,ater hteegsi ifrn unu rvttoa approaches. gravitational quantum different in and modified emerges Chern-Simons systems that on theory these particular a by in gravity, emitted concentrate We signals LISA. the by advance detectability affect their can to interaction interest gravitational the of to modifications how also here discuss We are Antenna observatories. gravitational-wave Space (IMRIs ground-based Interferometer important inspirals Laser most Intermediate-mass-ratio future the the of (LISA). for one gravitational-waves is of (EMRIs), sources inspirals extreme-mass-ratio as known ally Abstract: Keywords: Eprint: Authors: with Gravity of LISA Theories Alternative of Tests Towards lmest eo enlssrs a lob infiatna h SOadin and ISCO the near significant be also can stress stress the Reynolds where horizon, event zero. the fea- outside to no just plummets (exhibiting until radii ISCO) all the at with inward associated ture smoothly and rises thickness It disk topology. both magnetic of in- poloidal independent approximate completely fluid-frame almost of in is radial-dependence is stress time-averaged flow electromagnetic the accretion that aver- find the We and when equilibrium. devoted extent, time-periods flow was azimuthal those care and over much resolution only cases, adequate all aging ensuring In topology. issues: magnetic dependence technical on possible to stress investigate disk to inner sim- order reported the in previously of spacetime two Schwarzschild with a simulations these in H/R contrast ulations in We range a 0.17. span to allows simulations 0.06 our which H/R; from ratio, HARM3D, aspect simulations disk code these the conservative of of regulation intrinsically careful Five 3-d the employing spacetime. with all Schwarzschild performed simulations, a were of in number MHD a relativistic of general results the contrasting by accretion Abstract: holes black supermassive parts; Keywords: Eprint: Authors: parame- on case stress Schwarzschild the disk ters: accretion inner of Dependence http://arxiv.org/abs/1001.4809 http://arxiv.org/abs/1001.4899 oura alsF;Yns Nicolas Yunes, F.; Carlos Sopuerta, ol,SotC;Koi,Jla . aly onF. John Hawley, H.; Julian Krolik, C.; Scott Noble, eepoeteprmtrdpnec finrds tesi lc hole black in stress disk inner of dependence parameter the explore We h nprlo tla opc bet nomsiebakhls usu- holes, black massive into objects compact stellar of inspiral The MI eea eaiiy rq;hpt;IR;tsso lentv theories alternative of tests IMRI; hep-th; gr-qc; relativity; general EMRI; crto ic;atop.O sr-hH;atohsc;E counter- EM astrophysics; astro-ph.HE; astro-ph.CO; discs; accretion o tr itiueaon asv lc hole black massive a around distribute stars How

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 oetmacee e ntrs-as71%ls hnteaglrmmnu of momentum angular the than less ISCO. 7-15% the angular rest-mass disk net unit the both make per on to accreted depends combine momentum stresses however, two stress, The topology. this magnetic of and thickness magnitude the region; plunging the e,dsusisrlto ihncercutr nohrglxe,adpitotwhere out point and galaxies, other needed. clus- in is star clusters research nuclear nuclear further Way resolve with Milky can relation the of its we in knowledge discuss which population current ter, kind and our dynamics, its summarize structure, will of its I nuclear one study detail. can understanding only we the for Thus, is template stars. black it individual unique into massive because a the general is surrounds in cluster that clusters Way, This star Milky knowledge the nu- A*. current of the Sagittarius our center introduce hole, of the will I at overview Subsequently, cluster brief formation. their star a their in clear give and cluster will clusters star star I massive nuclear article, most on and this densest In the galaxy. usually are host They galaxies. of ity Abstract: Keywords: Eprint: Context Authors: in Cluster Star Nuclear Way Milky The singular point-like with equations of solutions problems numerical of avoid differentiability behaviour. we particle low time, a the same of the to presence at the avoid due and, with we way, domain associated this computational scale In length the small in them. a two subdomains resolving betweem of several of interface into feature need the domain the principal at spatial The particle the the of geometry. locating division and Schwarzschild the a in consists in method particle our scalar a on acting Abstract: Keywords: Eprint: Authors: Pseu- using Methods dospectral Inspirals Extreme-Mass-Ratio Modelling http://arxiv.org/abs/1001.4238 http://arxiv.org/abs/1001.4697 codl Rainer Schoedel, F. Carlos Sopuerta, Priscilla; Canizares, ula trcutr r oae ttednmclcneso h major- the of centers dynamical the at located are clusters star Nuclear eitoueanwtm-oanmto o optn h self-force the computing for method time-domain new a introduce We sr-hG;atohsc;osrain;SgtaisA* Sagittarius observations; astrophysics; astro-ph.GA; waveforms force; self gr-qc; relativity; general EMRI; o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW

61 oe esfrG science GW for News & Notes Notes & News for GW science 62 WNotes GW a asfnto fteds tr seteeytphaywt etfi power fit best a with top-heavy extremely a is observe stel- stars We The disk puzzling. of disks. the is law the which of arcseconds, outside function few distribution mass central isotropic the lar in more stars a late-type of in dearth be to seem 12" Sgr on igesa omto event formation star single a hyaecmail ihasadr aptrKop M bs tpwrlwof law power fit (best IMF IMF; disk Salpeter/Kroupa the standard from a of dN significantly and with differ 0.8" compatible 12" inside are beyond S-stars they distances the of at functions stars mass early-type The the (IMF). function mass initial the 12" and re- 0.8" stars between B- disks and 0.36+/-0.06) O- = (WR), ( fide Rayet eccentric bona Wolf Sgr from warped 177 these strongly of of two sample most in total that side a find We in result stars. spectro- which ESO/VLT, early-type field integral the assisted, on optics adaptive SINFONI the graph with Galaxy the of parsec central Abstract: Keywords: Eprint: Authors: Center Galactic the in Stars Young Massive oiydsrbto a ernoie ytevlct ik u ofebc from rotating gaseous feedback of ve- to simulations gas due hydrodynamical the kicks perform bulges velocity we inside the Here de- by Indeed, the formation. large, randomised star significant. be be to be can likely also distribution very can locity is mean bulge the the from in viations However, momentum angular momentum. mean angular specific the large while is (SMBHs) holes black supermassive Abstract: holes black sive Keywords: Eprint: Authors: holes black supermassive feed- of the ing in turbulence supernovae-driven of role the On / dm A ∼ dN http://arxiv.org/abs/1001.3883 http://arxiv.org/abs/1001.4232 ∗ m A h ae yeBsas(K;5 nterda nevlbten08 and 0.8" between interval radial the in (mK&;15) stars B type later The . ato H. Bartko, ob,Aeadr aasi,Sre;Pwr hi;Kn,Andrew King, Chris; Power, Sergei; Nayakshin, Alexander; Hobbs, thsln enrcgie httemi btcet crto fgsonto gas of accretion to obstacle main the that recognised been long has It − / esmaieorlts bevtoso h ula trcutri the in cluster star nuclear the of observations latest our summarize We ∗ 2 swl sacnrlcmatcnetain(h -trcutr centered cluster) S-star (the concentration compact central a as well as , dm sr-hG;atohsc;osrain;SgtaisA* Sagittarius observations; astrophysics; astro-ph.GA; crto ic;atop.O sr-hH;E oneprs supermas- counterparts; EM astro-ph.HE; astro-ph.CO; discs; accretion . 15 + ∼ / m − 0 o tr itiueaon asv lc hole black massive a around distribute stars How − . 3 0 . . 45 + / − 0 . 3 ic tlatteW/-tr eefre nst in situ in formed were WR/O-stars the least at Since . ∼ ysao hsms ucinpoal reflects probably function mass this ago, Myrs 6

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 ai . c h lc oe omn nteedne ihrdhf lsescan clusters redshift high dense, these in forming holes range black the black of in The time masses have the pc. at 0.5 clusters < stellar most radii the nuclear among the (z collisions for formation the runaway hole masses for from Typical environment ensuing suitable seed, stars. a hole massive provides black the cluster a from of stellar inflowing gas formation nuclear from The starburst central fragmentation. a for disc. of metallicity result unstable a critical as the forms above cluster nuclear just A metals with polluted been has a be can bulges in via formation gas star accretion. the that SMBH channel for argue to catalyst therefore need strong We the bars. without fuel or to provide of discs results could supply large-scale our accretion sufficient Rescaling of a mode with few. "ballistic" SMBHs a this the of that factor argue di- a we simulations bulges, within the astrophysical that to of formula results analytical boundary numerical simple the innermost a derive captures the we approximation, impact and ballistic to turbulence, the without Using gas rectly. simulations of the fraction in found a was allows that prevents mixing This gas drag. travel hydrodynamical efficient by flows, the unaffected "ballistic" turbulent largely of gas convergent notion ambient by of the the created through orders on based filaments, several understood dense to be whereby up can accretion, by this rate rate, that accretion accretion show We low this a efficient increases magnitude. in to turbulence resulting leads of momentum, process inclusion angular circularisation the different the with imple- case gas We rotating of find purely mixing We hole. the spectrum. black velocity in turbulent the while supersonic from a velocity that, of distances of means large by importance dispersion relatively the this at ment quantify gas to the attempting in SMBH, dispersion an onto infalling shells salse ttemmn fterfrain ehr oe h vlto fhigh of temperatures evolution that virial the with holes halos model matter black here explore dark We and in we hosted formation. clusters paper discs, their redshift star this of nuclear In moment the between galaxies. at connection establishes few a shown a of have least possibility investigations at the in Recent co-exist clusters. components stellar both nuclear that or holes black massive Abstract: holes black Keywords: Eprint: Authors: mas- description central model of I: objects evolution sive and formation redshift High http://arxiv.org/abs/1001.3874 eeci . ootr,M;Cli . art F. Haardt, M.; Colpi, M.; Volonteri, B.; Devecchi, aatcnce otcnrlmsieojcsete ntefr fsuper- of form the in either objects massive central host nuclei Galactic crto ic;atop.O srpyis omlg;supermassive cosmology; astrophysics; astro-ph.CO; discs; accretion o tr itiueaon asv lc hole black massive a around distribute stars How ∼ 0 r nh range inthe are 10) ∼ 0-00slrmasses. solar 300-2000 WNotes GW 10 4 − 10 6 oa assadhv afmass half have and masses solar 10 4 ,woegas whose K,

63 oe esfrG science GW for News & Notes Notes & News for GW science 64 WNotes GW e prahfrgnrtn yrdps-etna ueia aeom for waveforms Numerical / systems. post-Newtonian challenging these hybrid generating a for introduce and approach binaries, new black-hole highly-precessing, generic, of simulation linear Abstract: theory Newtonian Keywords: Eprint: Hans-Peter Bischof, Yosef; Zlochower, Hiroyuki; Authors: Bina- Black-Hole Generic ries of Simulations in Advances asclbaina h ee fafco fafew. a of overall factor the a affect of could level that the systematics at potential calibration still mass scatter, are intrinsic there little that however, surprisingly note, have to bulge seems host-galaxy the also and that luminosities masses find hole also We black reverberation-based measurements. between reverberation the relationship better between the in relationship uncertainties the small, the very in is to size scatter and region broad-line intrinsic mapping the the and reverberation luminosity that from AGN find results We to holes attention limitations. black special their supermassive with on attention nuclei, focus active then in and nuclei, galactic in holes black Abstract: holes black Keywords: Eprint: Authors: Hole Black Central Masses of Measurement Precision Toward http://arxiv.org/abs/1001.3675 http://arxiv.org/abs/1001.3834 eesn rde M. Bradley Peterson, erve reydrc n nietmtoso esrn h assof masses the measuring of methods indirect and direct briefly review We apnli aul;Lut,Cro . udm rn . Nakano, C.; Bruno Mundim, O.; Carlos Lousto, Manuela; Campanelli, erve oeo h eetdaai eeomnsi h ul non- fully the in developments dramatic recent the of some review We sr-hC;atop.A srpyis bevtos supermassive observations; astrophysics; astro-ph.GA; astro-ph.CO; rq;msiebnre fbakhls ueia eaiiy post- relativity; numerical holes; black of binaries massive gr-qc; o tr itiueaon asv lc hole black massive a around distribute stars How a 1 2010 21, May ∼ .1dx comparable dex, 0.11

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.7dx We dex. 0.17 oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 rtdb OpenCL by erated accel- sources wave gravitational of modeling Numerical hsmksi osbefraybnr asv lc oe omrewti Hubble a ratio. within merge Eddington that to and holes ﬁnd ratio black We mass massive binary the time. any on for dependent possible only it makes but This mass of massive order hole (2009). the black binary as Hayasaki the of estimated by of is evolution proposed decay of orbital disks of theory gaseous timescale ambient the The with on massive interacting binary based holes of AGNs function black nearby mass the in study binary We holes harbor centers. should black AGNs their of in fraction holes signiﬁcant black a massive then mergers, galaxy major by Abstract: Keywords: Eprint: Authors: Active in holes black Nuclei massive Galactic binary of function Mass Abstract: Keywords: Eprint: Authors: n/rSitBrtAetTlsoe ls iaiswt oa lc-oemse of AGNs. masses Image black-hole X-ray total All-sky with binaries of 10 Close Monitor Telescope. as Alert such with Swift/Burst detectable monitors and/or ten-years, X-ray than sensitive less highly period on-going orbital with black-holes massive binary rhtcue n e bansrn efrac an htaecmaal owhat SDKs. to native comparable Cell the are from both that and derived on gains be source-code CUDA can performance identical strong native execute obtain with to yet the us and them on architectures allows compare framework based OpenCL then implementations The and previous SDKs. results, our performance ap- from parallelization our Tesla our those present and and detail, BE technologies Cell in compute – proach these accelerators describe We hardware GPU. the CUDA using application modeling EMRI 6 . 5 − 7 M http://arxiv.org/abs/1001.3612 http://arxiv.org/abs/1001.3631

aaai iiae ea ohhr;Ioe Naoki Isobe, Yoshihiro; Ueda, Kimitake; Hayasaki, Justin McKennon, Gaurav; Khanna, r h otfeun nmsiebnr lc-oeppltoso nearby of populations black-hole binary massive in frequent most the are fteatvt fatv aatcnce AN)i rdmnnl induced predominantly is (AGNs) nuclei galactic active of activity the If nti ok emk s fteOeC rmwr oaclrt an accelerate to framework OpenCL the of use make we work, this In sr-hC;atop.A srpyis asv iaiso lc holes black of binaries massive astrophysics; astro-ph.GA; astro-ph.CO; aaaayi;ER;GU rq;physics.comp-ph gr-qc; GPU; EMRI; analysis; data o tr itiueaon asv lc hole black massive a around distribute stars How 1 . 3% − − 1 . 7% ftettlnme fnab Gshv close, have AGNs nearby of number total the of WNotes GW 10 8 yr en independent being ,

65 oe esfrG science GW for News & Notes Notes & News for GW science 66 WNotes GW Abstract: Keywords: Eprint: Authors: cooling radiative with flows cretion ac- hot of simulation hydrodynamical Two-dimensional uioiydsac,ti ol lo st infiatycntantedr energy dark the constrain significantly the to of parameter measurement us the equation-of-state allow with could Combined this finding redshift. distance, its of luminosity obtaining chances and the galaxy improving cos- host dramatically the precision localization, for allows sky signal tool inspiral high-accuracy new the for in a harmonics signal provide sub-dominant could of Inclusion (SMBBH) mography. holes black binary massive Abstract: Keywords: Eprint: LISA with Authors: state of equation energy dark the Measuring increases still direction decreases. flow. gravitational entropy the non-radiative of radial in gradient of the entropy the case and although of the inward gradient unstable, to the convectively hole compared because strongly black little is of still changes This evolution is rate the flow accretion and the of hole, profile that black find of We growth appear- observational the spin. the flows, determines accretion rate of accretion mass ance the of profile the important is because performing problem by This cooling radiative simulation. strong numerical of hydrodynamical presence correspondinglytwo-dimensional the and in instability rate accretion convective of regime. the profile than flow the investigate accretion stronger hot we paper, becomes luminous the present radiation in- into the enters the In slower flow when the increase i.e, decrease will heating, even viscous entropy the can the entropy radiative important, The the more When convective ward. and the simulations. in more these lost in outer becomes is neglected the rest cooling a usually at the is while is available hole, Radiation gas rate black accretion accretion the outflows. of mass onto fraction the fall small finally of its can a profile of boundary only the because i.e., result, unstable, radius, a convectively of As is function flow entropy. the of that increase is inward flows accretion hot of tions http://arxiv.org/abs/1001.3099 http://arxiv.org/abs/1001.3571 un eg u Defu Bu, Feng; Yuan, rek hi a e;Tis . aharks,B . its .M. A. Sintes, S.; B. Sathyaprakash, M.; Trias, Den; Van Chris Broeck, h otipratfidn ftodmninlhdoyaia simula- hydrodynamical two-dimensional of finding important most The h ae nefrmtrSaeAtnas(IAs bevto fsuper- of observation (LISA’s) Antenna’s Space Interferometer Laser The crto ic;atop.O sr-hH;E oneprs spin counterparts; EM astro-ph.HE; astro-ph.CO; discs; accretion srpyis omlg;g-c asv iaiso lc holes black of binaries massive gr-qc; cosmology; astrophysics; o tr itiueaon asv lc hole black massive a around distribute stars How w vnwt igeSBHmre at merger SMBBH single a with even a 1 2010 21, May z .

1 Such . oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 neetcnptnilyhv opnn assfo ierne( range wide a from masses component have potentially can event an eosrtsta mohmdfidsuc em olf h otslto n re- and solution Jost it the and mollify radiation. measurements, terms junk types duce source self-force both modified and of smooth waveforms, influence that contaminates the perturbations, demonstrates studies which metric work solution, on This junk junk times. Jost of long the for solution as physical to persistent the referred a of here development solution, data: observe spurious initial junk We of trivial "burst" of domain. a consequence computational to unintended the leads another off choice propagates this ini- eventually known, is a well which which is radiation is solution As data a time. initial in in resulting discontinuous trivial and tially of inconsistent specification being despite unknown, initial choice, is correct common systems the because generic-orbit initial However, for an data. as data initial equation requires wave master problem a value of boundary forced solution distributionally Numerical by equations. described wave are master systems (EMRB) binary ratio mass extreme Abstract: Keywords: Eprint: Authors: of binaries modeling ratio time-domain mass extreme in solutions junk Persistent potential. full LISA’s of advantage take to required be accuracy would the effects degrade bi- severely Galactic will which from errors with background is lensing-induced distance confusion weak luminosity the However, the and measuring naries. noise in instrumental error LISA’s only the to that if due find cases, We most be in can errors. percent position of how few sky investigate estimation the also of the We knowledge into a identified. folded when be improve can parameters all galaxy on host accuracies the when measured be can Authors: Theory Numeri- Perturbation meets Binaries: Relativity cal Hole Black Ratio Mass Intermediate oaiain eedn nteprmtr ftesuc,ad(i o accurately how (ii) sky and for source, allow the mergers of SMBBH parameters possible the of on fraction depending what localization, (i) study understand in-depth an to perform order We in considerably. vary accuracies parameter which over Manuela http://arxiv.org/abs/1001.2578 il,SotE;Hshvn a . a,SehnR. Stephen Lau, S.; Jan Hesthaven, E.; Scott Field, ntecneto ercprubto hoyfrnnsinn lc holes, black non-spinning for theory perturbation metric of context the In oso alsO;Nkn,Hryk;Zohwr oe;Campanelli, Yosef; Zlochower, Hiroyuki; Nakano, O.; Carlos Lousto, MI rq;nmrclrltvt;sl force self relativity; numerical gr-qc; EMRI; w a eotie,epaiigta ehd omtgt eklensing weak mitigate to methods that emphasizing obtained, be can o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW w a emaue owti a within to measured be can 10 5 − 10 8 M

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67 oe esfrG science GW for News & Notes Notes & News for GW science 68 WNotes GW h osblt htortcnqecnb xeddt rdc cuaewaveform accurate simulations. numerical produce fully-nonlinear to of and extended number analysis modest be a data can from technique LIGO/VIRGO templates our for that techniques possibility these the q=1/10. of for waveforms applications compute discuss we We proof-of-concept, a leading As and the modes. for trajectories radii nonleading numerical large and nonlinear at of waveforms use compute to makes evolutions that perturbative technique efficient new a with 0.1 < q Abstract: relativity Keywords: Eprint: lc holes black Keywords: Eprint: Authors: time cosmic occu- over hole fraction black pation massive on effects recoil: Gravitational in even appear can density) pressure. mass magnetic small the ring- of a in limit that oscillations the is radial result (i.e., main The profile case. density general a like more with analysis the our of complete integration We numerical integrated pressure. direct magnetic be small can of equations limit resulting the in The analytically system coordinate. differential ordinary dimensionless physical an vertical relevant to the reduced the thus in of is system dependence The radial assumed. the is definite, quantities a for once form separated hyperbolic) be par- can In (or system disks. oscillatory differential accretion partial in the plasma that the show of we ticular, equilibria vertical and radial the describing Abstract: Keywords: Eprint: of Authors: Structure Oscillatory Disks the Accretion in for Plasma Solution Separable A http://arxiv.org/abs/1001.1743 http://arxiv.org/abs/1001.2430 http://arxiv.org/abs/1001.2316 ootr,Mra utkn ahn ot,Massimo Dotti, Kayhan; Gultekin, Marta; Volonteri, Giovanni Montani, Massimiliano; Lattanzi, esuybakhl iaisi h nemdaems-ai eie00 < 0.01 regime intermediate-mass-ratio the in binaries black-hole study We epoieanwaayi ftesse fprildfeeta equations differential partial of system the of analysis new a provide We sr-hC;atohsc;csooy ik/eol asv iaisof binaries massive kicks/recoil; cosmology; astrophysics; astro-ph.CO; crto ic;atop.R srpyis Mcounterparts EM astrophysics; astro-ph.SR; discs; accretion rq;msiebnre fbakhls ueia ehd;numerical methods; numerical holes; black of binaries massive gr-qc; o tr itiueaon asv lc hole black massive a around distribute stars How

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 Abstract: bandi h I n -a eiea ela h o eeto nterdodo- radio the in detection non the as profiles well flare as the regime of X-ray main. widths and expansion different from NIR adiabatic and the covered with in luminosities was combined obtained peak that model related 2007 SSC the April the explain 4 domain, can of X-ray brightest event the the flare to to bright radio lowest the the the For from emission SgrA*. all from for flare responsible wavelengths is near-infrared from at mechanism that emission SSC conclude We ob- the SSC domain. variations X-ray state density continuous and flux NIR luminosity a the the for high in from account served the fully emission can For components synchrotron source peaked as disk. THz interpreted accretion spotted be even can or dur- state luminosity A* The low Sagittarius states. the of luminosity counterpart observed ing highest (SMBH) and hole lowest black its near massive (SgrA*) super the of curves light Abstract: Keywords: Eprint: Za- C.; Straubmeier, R.; Schoedel, A. K.; Zernickel, M.; Muzic, maninasab, D.; Kunneriath, M.; Garcia-Marin, R.; Authors: A* Sagittarius of states luminosity extreme The iteefc ntefeunyo Bsi ag aais(tms 0 effect). 20% a most (at galaxies large in MBHs of frequency can to the Recoils galaxies on small effect wells. in little for- MBHs potential MBH of shallow frequency hierarchy: such overall merger the in decrease MBH formation inefficient the galaxy likely but are their probability, processes along ejection mation low high poten- very a shallow is have with rate velocities, halos, merger escape Small low fraction. plays and efficiency, retention wells formation the tial MBH increasing and in bias frac- role halo ’occupation crucial to The a related galaxies. intimately in a today MBHs, continuously MBH host of a form z>5-7 host tion’ MBHs to at unless galaxy) 50%, halos size than similar all less (or if Way is are Milky that the which find of mergers, We probability gas-rich the ’wet’, MBH, galaxies. ’aligned’ for high-redshift situation the for realistic with expectation most case the the this is contrast latter We The configuration distributed. case. spin/orbit isotropically the be and coa- to processes, binary expected dynamical MBH is stellar the where by environment, driven probabil- gas-poor is ejection a lescence assess in We occurring MBHs. mergers of on for fraction’ function and ities ’occupation bias, a the cosmic as on halo MBHs reflects host for the that recoil of how and the configurations of spin/orbit ’danger’ MBH of different the history of discuss merger We cosmic the population. along MBH recoil, the radiation gravitational the to due centres, http://arxiv.org/abs/1001.1351 ah,N;Wte,G;Ekr,A;Bchl,R . rmr . Giessuebel, M.; Bremer, M.; R. Buchholz, A.; Eckart, G.; Witzel, N.; Sabha, eass h nuneo asv lc oe(B)eetosfo galaxy from ejections (MBH) hole black massive of influence the assess We edsusm-aeeghrdo .-18mNRad21 e X-ray keV 2-10 and NIR 2.2-11.8um radio, mm-wavelength discuss We crto ic;atop.A srpyis bevtos aitru A* Sagittarius observations; astrophysics; astro-ph.GA; discs; accretion o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW ∼ 0,wiete have they while 60%,

69 oe esfrG science GW for News & Notes Notes & News for GW science 70 WNotes GW eutwudms ieyselteedo TEVES/MOND. of end null the a spell assumptions, exist. likely standard they most on would should based result detail, signal some predicted in large the characterised gradiometer not given and Conversely, the will measured gradients if but these that detected, performance, be conclude nominal just and its achieves to, gradients spacecraft gravity exposed the MOND be on-board the should of in- preferred Pathfinder estimates probably the robust LISA year, present one that that We order conclude fly-by. of lunar and times exam- a transfer point, We volves short saddle relatively gradients. the in gravity reach resulting anomalous strategy, to fly for strategies to look following is to various point, concept order ine saddle in basic Sun-Earth The mission, the nominal around time. its region years’ the few through direct, a Pathfinder a just LISA to in incorporates, test, it experimental phenomenology controlled MOND non-relativistic the particular Abstract: Keywords: Eprint: Authors: Pathfinder LISA with MOND/TEVES Testing sda xdpit fteslto:11,14,15,17,18,18,19,2005 orbit. of 1995, the mass of 1984, primary 1 parameters the 1983, are eight 1973, these of of 1957, determination interesting the 1947, Most allows 1913, historical This the solution: outbursts. both the 2007 been and of from have points outbursts measurements fixed photometric Nine solution recent as from exact used limits. as an error well allows as tight identification records very This major photographic with as OJ287. identified orbit, are of the times curve of These light times. the specific in at which outbursts secondary disk accretion the an by has impacted primary the is that assumed is It secondary. non-spinning Abstract: spin observations; Keywords: R. Eprint: Saunders, M.; Basta, R.; Hudec, H.; Rampadarath, A.; Gopakumar, D.; Authors: OJ287 in Spin Hole Black Measuring . 46 · 10 http://arxiv.org/abs/1001.1284 http://arxiv.org/abs/1001.1303 8 M rne,Crsin ebe tv;Bvs el auio Joao Magueijo, Neil; Bevis, Steve; Kemble, Christian; Trenkel, atnn . ikl,S;Lho .J;Hvnn . iso,K;Merritt, K.; Nilsson, T.; Hyvönen, J.; H. Lehto, S.; Mikkola, M.; Valtonen, emdltebnr lc oesse J8 sasinn rmr n a and primary spinning a as OJ287 system hole black binary the model We esgetta IAPtfidrcudb sdt ujc EE,adin and TEVES, subject to used be could Pathfinder LISA that suggest We

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h eodr mass secondary the , oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 ikbtenteselrms n ue-asv lc oepopulations. hole black super-massive missing and after mass sought stellar long the the between providing the of link holes, for hole black date black to mass evidence the intermediate observational of of strongest existence mass the the presents finding of This limit maximum Msun. lower 500 a conservative with implied source an X-ray to with variable 243-49, up a of of luminosity dispute, detection de- keV in as the 0.2-10 accepted is report widely holes we are black Here none mass proposed, finitive. intermediate been have such candidates of many existence though The and Sun. the of that ue-ipytepeec fa crtn lc oewt asof mass a with pres- hole black gravitational Ed- accreting the an by of (i.e. presence balanced theoretical the is the imply pressure - below sure radiation and the isotropic where is limit, emission dington) the if - luminosities treme value Einstein’s with agree to found sigma). is (1 energy rate 2% orbital loss of of accuracy The the loss with the waves. measured gravitational also to have We due precision. achievable the within is parameter spin dimensionless The 0.70. orbit ulu ftehs aaywt ooercluminosities bolometric with galaxy host the of nucleus Abstract: observations Keywords: Eprint: Joana Solar 500 Authors: Over 243-49 ESO of Galaxy the Hole in Masses Black Intermediate-mass An value Einstein’s the of sigma) Authors: Mergers Galaxy in Inflows Gas Multi- Scale via Holes Black Supermassive of Formation Direct pni .1 ehv lotse h osblt htteqarpl emi the a in theory: term Einstein’s quadrupole follow the the exactly that if not 2015 possibility does November the motion 26 parameter tested on of and also equations middle 0.25, have the Newtonian is We in Post spin is the value 0.31. if spin 2016 is the January spin due. if 3 is on 2015 outburst range, December next this 15 the of on when begin 2015 should in outburst constrained The tightly more be will parameter http://arxiv.org/abs/1001.0567 ae,Lco aatii,Seis saa nrs algr,Simone Callegari, Andres; Escala, Stelios; Kazantzidis, Lucio; Mayer, lr-uiosXrysucsaeetaaatcojcslctdotiethe outside located objects extragalactic are sources X-ray Ultra-luminous arl,Sa;Wb,Ntle art iir oe,Oiir Rodrigues, Olivier; Godet, Didier; Barret, Natalie; Webb, Sean; Farrell, q sr-hC;atop.E srpyis nemdaems lc holes; black intermediate-mass astrophysics; astro-ph.HE; astro-ph.CO; sitoue soeo h aaees t au swti 0 (1 30% within is value Its parameters. 8 the of one as introduced is o tr itiueaon asv lc hole black massive a around distribute stars How q = 1 . 2 1 hsspot the supports This . × 10 WNotes GW 42 erg s − 1 nteeg-nsia aayESO galaxy spiral edge-on the in 0 . 28 no ± − > hairtheorem 0 . 10 01 39 1sga.Telast The sigma). (1 erg ∼ 10 s fbakholes black of − 2 1 hs ex- These . − 10 5 times ∼

71 oe esfrG science GW for News & Notes Notes & News for GW science 72 WNotes GW ilo oa assi esta ilo er yaceiggsfo h surround- the a from to gas grow accreting can by years hole billion black a The disk. than ing hole. less black one in massive in masses a solar cloud of billion even- scale formation which sub-parsec the collapse, a to gravitational leads in undergoes tually gas cloud of The masses years. accumu- solar thousand inflow hundred gas million second 100 a than disk the more produce Within lates inflows disk. gas gas Merger-driven nuclear massive formation. unstable, star mergers an suppress that to accumu- show need gas no to central with required simulation lation the numerical enrich- produce a metal naturally protogalaxies rapid use cool massive the we between with not Here contrast does in protogalaxies. stars, that of into gas ment turned metal-free not the is requires at thus this gas and However, of efficiently collapse pri- direct of protogalaxies. by collapse of form the may center by holes gas inefficient black form to these seeds due Alternatively, appearance hole accretion. rapid black their explain light cannot which stars after metal-free in years mordial billion Models a than Bang. less Big place in the already were (SMBHs) holes black permassive Abstract: holes Keywords: Eprint: ii.Smlryt h etpril ii ae hnw etitteEBdnmc to dynamics EOB the test-particle restrict the we in when case, couplings limit spin-orbit test-particle all the reproduces to Similarly it order, limit. Also, 2.5PN the through reproduces mass-ratio. coupling spin-orbit any Hamiltonian the for EOB and When coupling the spin-spin orders, order S*. leading (PN) to post-Newtonian proportional interaction in spin-dependent expanded interacts additional particle effective an the spin and Thus, (having teraction S*. particle background spin effective Kerr a effective with the also the endow but with m, we mass descriptions, a with previous only in not As spinning for Hamiltonian binaries. particle’s (EOB) the effective-one-body black-hole in improved order an linear out at work spacetime, we curved spin, in particle test spinning a of tonian Abstract: waveforms spin; relativity; Keywords: Eprint: Authors: binaries black-hole spinning for Hamiltonian effective-one-body improved An http://arxiv.org/abs/0912.3517 http://arxiv.org/abs/0912.4262 aase nio unno Alessandra Buonanno, Enrico; Barausse, bevtoso itn rgtqaassgetta ilo oa assu- mass solar billion that suggest quasars bright distant of Observations uligo eetppri hc ecmue h aoia Hamil- canonical the computed we which in paper recent a on Building fetv n oy rq;msiebnre fbakhls numerical holes; black of binaries massive gr-qc; body; one Effective crto ic;atop.O Mcutrat;sprasv black supermassive counterparts; EM astro-ph.CO; discs; accretion o tr itiueaon asv lc hole black massive a around distribute stars How a 1 2010 21, May S Kerr

hog edsctp in- geodesic-type a through ) oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 lc-oebnre,a acltdi ueia eaiiysimulations. relativity numerical spinning in of calculated emission as gravitational-wave binaries, and black-hole are dynamics properties the the These in reproducing inspiral. maximum for the a crucial to and subsequent orbit, plunge circular the photon during frequency a existence orbital orbit, the circular as stable such innermost features, interesting an several of circular has which dynamics for EOB momentum, the angular exist, orbital orbits the with antialigned or aligned spins Keywords: Authors: non-precessing, holes black of equal-mass spinning, coalescence simulations: numerical relativity to calibrated waveforms Effective-one-body Abstract: forms Eprint: A. Mark Scheel, P.; Harald Pfeiffer, E.; Lawrence eiv httelre ifrnei h 32 oei u otelc fknowledge of lack the to modes. due higher is the We mode in effects case. (3,2) spin the anti-aligned post-Newtonian in spin of con- difference the larger spin in the both mode that (3,2) for believe lead- the modes and for the numerical amplitude except to good and considered, addition find EOB figurations We In the modes. between subleading 30-200Ms. agreements is four frequency mass arrival, compare of total we time mode, with (2,2) and binaries and ing phase for EOB initial the 0.999 the between than over overlap larger maximized the mode, that (2,2) LIGO find numerical Enhanced we the Using curves, noise case. while anti-aligned LIGO case spin Advanced aligned the and spin in ringdown. the errors and in numerical merger errors over during numerical slightly 10% within and is radians agreement dur- 0.4 equal-mass, 1% waveform to and The the and radians In 0.13 plunge, to and radi- reduced inspiral waveforms. 0.01 be ing can inspiral to differences entire reduced these case, the be anti-aligned can over spin respectively, mode 1%, (2,2) dif- EOB amplitude In and fractional and ans and numerical parameters. phase the that EOB-adjustable find between of we ferences errors case, handful aligned amplitude a spin numerical and equal-mass, calibrating between the phase difference by the the waveforms minimize estimate EOB then first and and we waveforms 1000M, numerical frequency the of low in interval at non-precessing waveforms time numerical spinning, a and over EOB of the Aligning simulations binaries. numerical-relativity black-hole accurate to model http://arxiv.org/abs/0912.3466 a,Y;Boan,Aesnr;Bcmn us . h,Tn;Kidder, Tony; Chu, T.; Luisa Buchman, Alessandra; Buonanno, Yi; Pan, epeettefis tep tclbaigteefcieoebd (EOB) effective-one-body the calibrating at attempt first the present We fetv n oy rq;msiebnre fbakhls pn wave- spin; holes; black of binaries massive gr-qc; body; one Effective o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW

73 oe esfrG science GW for News & Notes Notes & News for GW science 74 WNotes GW H(at BH F tdfeetglci uli ula Fi oetgtyculdt G activity, AGN to coupled scales. and tightly all more BHAR at is between exist SF correlations correlations nuclear but predict nuclei: We the galactic and gas. different formation at and star SFR stars including the requires both mode of this sub- self-gravity of to treatment a gas the Proper to driving unstable (m=1), scales. becomes mode pc spiral gas single-armed the a However, or disk present. eccentric longer standing, no are modes mor- bar-like nuclear and with accretion BH At correlate to phology. attempts duty complicating their modest, bars; is and clumps, cycle rings, spirals, including morphologies, diverse exhibits to up gravi- of of rates series accretion a large systems, generates disk-dominated instabilities gas-rich, tational sufficiently bar-(un)stable isolated For We and ( mergers galaxies. nuclei physics. major disk both galactic ISM including of the simulations, simulations for scale our galaxy models for subgrid star conditions and self-gravity, initial properties (BHs), generate galaxy holes use of black We space stars, rameter gas, feedback. accre- are stellar Keplerian ingredients traditional and a key formation, resemble The to begins disk. gas the tion where <0.1pc, to scales tic Abstract: holes black supermassive counterparts; EM Keywords: Eprint: Gas? Authors: Their Get Holes Black Massive Do How ais eciigteotraceinflwtgte ihteifligrgo.The region. infalling the gravitational with (BH) together hole flow black accretion to outer arcseconds Chandra the several X-Ray describing from quiescent radius, extends extensive model to The emission bremsstrahlung data. the fit and A* Sgr Abstract: holes black massive Keywords: Eprint: Authors: Con- A* and Sgr Winds near duction Stellar with Solution Inflow-Outflow < http://arxiv.org/abs/0912.3255 http://arxiv.org/abs/0912.3257 ∼ okn,Pii . utet Eliot Quataert, F.; Philip Hopkins, hhrao,RmnV;Bgnf,FeeikK. Frederick Baganoff, V.; Roman Shcherbakov, euemlisaeSHsmltost olwteiflwo a rmgalac- from gas of inflow the follow to simulations SPH multi-scale use We epooea2tmeauerda yaia oe fpam o near flow plasma of model dynamical radial 2-temperature a propose We 0c u iuain eebete’aswti as oe,bttegas the but model, bars’ within ’bars the resemble simulations our 10pc, crto ic;atop.E Mcutrat;SgtaisA;super- A*; Sagittarius counterparts; EM astro-ph.HE; discs; accretion crto ic;atop.O sr-hG;atop.E astrophysics; astro-ph.HE; astro-ph.GA; astro-ph.CO; discs; accretion ∼ -0c h rvttoa oeta eoe oiae yteBH the by dominated becomes potential gravitational the 1-10pc, o tr itiueaon asv lc hole black massive a around distribute stars How ∼ 0 iuain osre ag pa- large a survey to simulations 100 a 1 2010 21, May 1 − 10 < M

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0p)using 300pc) y nothe onto /yr oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 ne o,tu iiga igemdlo g *aceinsial tayradius. any at suitable accretion A* Sgr of model single a at aiming thus flow, inner rfiepoe o te erteB,tu ycrto efCmtnpitsource point self-Compton synchrotron luminosity a with con- thus inferred thermal BH, brightness is the of X-Ray near effect The steep flow. the too turbulent to proves a due profile in rate The production Bondi entropy region. of by the 1% from enhanced below outflow duction to to found limited is is gas rate of accretion Most stagnation performed. the is for points search sonic Self-consistent separately energy. and considered and are momentum star mass, each of from particles sources winds as of Stellar capacity winds. stellar heat by relativistic feeding and conduction, heat electron incorporates model Eprint: Pietro Ubertini, Francesca; Panessa, Lorenzo; Fioc- Natalucci, Teresa; E.; Josh Maria Grindlay, chi, Paolo; Coppi, Fabrizio; Tavecchio, Giovanni; Pareschi, Luigi; the Authors: in Holes Black Super-Massive Universe of view EXIST The small. coordinates are the waves gravitational Although extracted position the problem. a in changes introduce this We the addresses change, binaries. that mass damping unequal shift in properly ac- mass not be dependent in does to difference parameter has the damping which constant for parameter, a count black damping However, a each evolutions. is stable near condition for coordinates shift chosen stationary the of approximately Part to hole. leads that choice gauge Abstract: relativity Keywords: Eprint: Authors: mass unequal simulations for binary hole condition black shift dynamical a Toward lc holes black Keywords: http://arxiv.org/abs/0912.3125 http://arxiv.org/abs/0912.3096 ule,Dre;Bugan Bernd Bruegmann, Doreen; Mueller, el ea oet;Gieln,Gbil;Tgifri inir;Foschini, Gianpiero; Tagliaferri, Gabriele; Ghisellini, Roberto; Ceca, Della oigpntr iuain fbakhl iaisrl naspecific a on rely binaries hole black of simulations puncture Moving rq;msiebnre fbakhls ueia ehd;numerical methods; numerical holes; black of binaries massive gr-qc; sr-hC;atop.E srpyis bevtos supermassive observations; astrophysics; astro-ph.HE; astro-ph.CO; o tr itiueaon asv lc hole black massive a around distribute stars How L = 3 x 10 32 r/.W ttesbm msinfo the from emission sub-mm the fit We erg/s. WNotes GW

75 oe esfrG science GW for News & Notes Notes & News for GW science 76 WNotes GW h eyfis MHi h nvrealwn st e togcntanso the on constraints strong set Universe. to the in us growth allowing early and Universe of formation appearance the SMBH the of in probe models to SMBH it first enables blazars, very rare the EXIST’s very least but not powerful, but find Last to blazars). power SMBH ability of accretion observations how between using link an (by of the power of iii) physics jet/outflow properties and and the AGN), variability of ii) and sample spectra significant Universe), and X-ray - unbiased heavily broad-band z<0.5 the measuring studying and - (by revealing local when accrete (by the i) Universe in the understanding: accretion in in obscured active progress are major SMBH enable instru- where will EXIST’s and EXIST of combination particular unique In the by ments. enabled topics science AGN amenable are selected ( that keV studies 10 follow-up above detailed detected to AGN of number will the and increase bottleneck dramatically previous identification overcome "multi-wavelength" will the break strategy time will this in biases, range; also selection energy but expanded space significant in just a not over activity, and SMBH of missions) X-ray prior and current MHpa nteUies.I atclrEITwl ar u nunprecedented an out carry that factor will role (a EXIST the keV particular and 10 In phenomenon above AGN survey Universe. the the of in study play the SMBH been tackle has conference) properly monitoring this to at all-sky Survey designed contribution Imaging keV), Natalucci L. X-ray (0.1-600 see Energetic (EXIST, X-ray proposed mission Telescope the soft/hard follow-up, to on-board micron) and capability, 2.2 to (0.3 cal/NIR Abstract: neetn osrit nti uniya ucino k oiinadredshift, and position sky of place function indeed a could as detectors quantity space-borne this that find on We constraints merger. interesting con- of Newton’s wave time of gravitational the time-derivative first at a the stant given on Such constraints and, for frequency. allow function they chirping response observation, the the in a into corrections to propagate to corrections constant leading Newton’s grav- luminosity, the of and wave energy promotion itational binding binary’s The the to waves modifications physics. introduces gravitational time-function fundamental their rendering of ratios, probes signal-to-noise ideal large high to with coalescences and hole black redshift observe to expected are Antenna, Space terferometer Abstract: relativity numerical Keywords: Eprint: Authors: observations wave gravitational con- with Newton’s stant of history evolutionary the Constraining http://arxiv.org/abs/0912.2724 ue,Ncls rtru,Fas pre,David Spergel, Frans; Pretorius, Nicolas; Yunes, pc-on rvttoa aedtcos uha h rpsdLsrIn- Laser proposed the as such detectors, wave gravitational Space-borne ihislrecleto ra ra-adeeg oeaefo opti- from coverage energy broad-band area, collection large its With sr-hC;atop.E omlg;gnrlrltvt;g-c hep-ph; gr-qc; relativity; general cosmology; astro-ph.HE; astro-ph.CO; o tr itiueaon asv lc hole black massive a around distribute stars How ∼ ∼ 00 G r xetd.W ics eeo few on here discuss We expected). are AGN 50000 0ices nhr -a estvt oprdto compared sensitivity X-ray hard in increase 20

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 oemresaeepce oocr IAosraino neulms inspiral equal-mass an measure of of to observation mass LISA redshifted A total with occur. event to expected are mergers hole a providing otIC igonApiue nEteeMs Ra- Inspiral Mass tio Extreme in Amplitudes Ringdown Post-ISCO op- vertically-integrated and H/R depth ratio corona tical aspect the with for “sandwich” models wedge different a three geometry: consider We a spectrum. producing power-law seed corona, photons X-ray thermal) thermal (but seed hard hot produces These a through surface. plane scattered disk inverse-Compton equatorial the then are BH to parallel our the oriented In in polarization relativity. with disk general photons thick full in optically code an ray-tracing model, Monte-Carlo a using (BHs), holes Abstract: Keywords: Eprint: Authors: Coronal Holes: Emission Black Accreting from Polarization X-ray Keywords: Eprint: Authors: -a oaiainsga rmsprasv H natv aatcnuclei. galactic active the in on BHs scattering paper supermassive coronal this from of of details signal effects bulk polarization the the consider X-ray the how also Although we models BH. show BHs, and We these stellar-mass corona on between focuses the sky. distinguish of the to properties of used various infer be plane and can the signal on spectropolarization the axis the as spin of defined to BH is energies direction the low vertical of the at projection peak; polarization thermal horizontal the radius above from BH polarization inner transition vertical the with characteristic on disk a a centered thermal find density, within truncated we uniform disk a of the by corona above surrounded spherical randomly and a distributed clouds and hot geometry; of wedge number finite a with http://arxiv.org/abs/0912.0907 http://arxiv.org/abs/0911.3899 cntmn eey rlk Julian Krolik, Jeremy; Schnittman, aa,Saa;Kl Barak Kol, Shahar; Hadar, epeetnwcluain fXryplrzto rmaceigblack accreting from polarization X-ray of calculations new present We G τ Mcutrat;aceindiscs accretion counterparts; EM MI rq;waveforms gr-qc; EMRI; ˙ osritmap constraint 0 / G osattruhu h ik nihmgnos“lmy corona “clumpy” inhomogeneous an disk; the throughout constant ttetm fmre obte than better to merger of time the at o tr itiueaon asv lc hole black massive a around distribute stars How vrteetr ag frdhfsweebnr black binary where redshifts of range entire the over 10 5 WNotes GW oa assfrtreyassol eable be should years three for masses solar 10 − 11 /yr. R edge nalcases all In .

77 oe esfrG science GW for News & Notes Notes & News for GW science 78 WNotes GW IAln-r interferometry long-arm LISA back- Schwarzschild the in equations differential ground. extract to (radial) reduces we ordinary which particular amplitudes, certain In ringdown solving black-hole waveform. associated emitted the the for expression for for an expression and an (ISCO) closed-form write in orbit We circular solution conditions). stable its initial of innermost independent the (somewhat from special trajectory is plunge The plunge. and Abstract: io uigfrtelclsto ftemxmm hr snntiildependence non-trivial requires quasi-circular is only a There parameter of maximum. direction the value of The the localisation the 15%. exceeds for by case tuning momentum minor this same in the energy with find roughly radiated We binary completes The varied. which is configuration direction a orbit. its for and one energy orbit, radiated quasi-circular in a maximum ini- of global the that a of to momentum fixed linear is the of data magnitude tial The relativity. general full in binaries Abstract: tivity Keywords: Eprint: Authors: orbits zoom-whirl low-momentum from Radiation associated to challenges developed been technical have the that them. techniques overcome on the and focuses measurements work long-arm these This with points spacecraft. three fiducial point between separate into measurement fiducial on long-arm a divided a and and be masses spacecraft, respective proof will their the baseline on between each measurements short-arm over two mil- measurement parts: five The approximately the of baselines in kilometers. over fluctuations lion masses picometer-level proof measuring drag-free by between band distance milliHertz the in radiation Abstract: Keywords: Eprint: Authors: http://arxiv.org/abs/0911.3862 http://arxiv.org/abs/0911.3175 od oa;Bugan Bernd Bruegmann, Roman; Gold, Ira James Thorpe, h ae nefrmtrSaeAtna(IA ilosregravitational observe will (LISA) Antenna Space Interferometer Laser The esuyzo-hr eaiu feulms,nnsinn lc hole black non-spinning mass, equal of behaviour zoom-whirl study We neteems ai nprlcnit ftoprs daai inspiral adiabatic parts: two of consists inspiral ratio mass extreme An rq;isrmns interferometers instruments; gr-qc; edscmto;g-c asv iaiso lc oe;nmrclrela- numerical holes; black of binaries massive gr-qc; motion; geodesic o tr itiueaon asv lc hole black massive a around distribute stars How

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 n upr ai da bu h fcec fgaiainlrdainfo binary a from radiation gravitational of efficiency system. the about being view Cor- ideas of While point basic physical support a minima). and discussed. from intuitive are and are merger findings maxima these before gauge-dependent, local shortly strongly (several dynamics eccentricity orbital with on relations radiated energy the of Authors: Relation Luminosity Spheroid - The Mass IV. BH Spheroids. and Holes Black of Evolution Cosmic electromagnetic of detection the in exploited waves. generat- gravitational be processes of can counterparts in and imprint their emissions epochs. leave detectable merger likely ing will and an features late-merge as dependent the in- well time during dynamics These as fields binary’s emissions electromagnetic the induced black of electromagnetically how orbiting enhancement possible show of in we pair variability particular, a a In by duce affected merger. are the fields through We vicinity. electromagnetic holes their the in how fields electromagnetic study and here plasmas radiation of (EM) behavior electromagnetic the of affecting emission induce by could system hole black binary a Abstract: relativity numerical Keywords: Eprint: Authors: fields electromagnetic effects on hole black Binary events: wave gravitational loud to counterparts electromagnetic possible Understanding Abstract: Keywords: Eprint: Blandford, Sarah; Gallagher, W.; Matthew D. Auger, Roger Le; Alexandre Bris, A.; Matthew bandwt h erIfae aeaadMliOjc pcrmtro board on Spectrometer Multi-Object and Camera Infrared Near the with obtained http://arxiv.org/abs/0911.3889 http://arxiv.org/abs/0911.4107 aezea als enr us ohd,Shin Yoshida, Luis; Lehner, Carlos; Palenzuela, nadto opouiglu rvttoa ae G) h yaisof dynamics the (GW), waves gravitational loud producing to addition In rmhg-eouiniae f2 efr- aaisa =.6adz=0.57 and z=0.36 at galaxies Seyfert-1 23 of images high-resolution From enr,Vrh ioa ru oms;Wo ogHk Malkan, Jong-Hak; Woo, Tommaso; Treu, Nicola; Vardha Bennert, sr-hC;atohsc;osrain;sprasv lc holes black supermassive observations; astrophysics; astro-ph.CO; sr-hH;E oneprs rq;msiebnre fbakholes; black of binaries massive gr-qc; counterparts; EM astro-ph.HE; o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW

79 oe esfrG science GW for News & Notes Notes & News for GW science 80 WNotes GW htmjrmresmypa h oiatrl ngoigshrisaoez above spheroids growing in role dominant indicating the relation, play this may follow redistri- not mergers a does major by sample that grows high-z spheroid the the However, that stars. or of relation bution fundamental more a either at hints ( mass the hole nu- of black spec- estimate morphology, Keck to luminosity. used host-galaxy spheroid is determine and troscopy luminosity we host-galaxy total (HST), luminosity, Telescope clear Space Hubble the iu ok.W loso httelclydfie nryo h trhsasimple a has order. star PN the 3.5 of the pre- energy to the defined up in mass locally derived its the motion with that of relation show equations also PN We 3.5 equa- the works. resulting with vious agree The fully stars. motion of non-rotating the tions symmetric of spherically motion orbital of the consisting describe describe done motion binary is to of computation equations limit The Our particle coordinates. functional. harmonic delta point in Dirac field the strong of instead the stars approx- using self-gravitating order relativity PN) general (3.5 to post-Newtonian imation third-and-a-half the through binaries pact Abstract: Keywords: Eprint: strong Authors: the using limit particle binaries point compact field relativistic for tion mo- of equations post-Newtonian order Third-and-a-half Interest- assembly. spheroid The precedes CL). the 95% growth ingly, at BH dex that (<0.6 suggests dex trend 0.3+/-0.1 evolutionary is or- redshift, two with over constant assumed to relation, range mass in BH cor- resulting mass the magnitude, BH extend of and ders we luminosity calibration, with self-consistent literature, a the to from rected taken z=4.5 to V- out present-day quasars fixed 44 at that luminosity, determine spheroid we effects, band evolution selection luminosity account into passive taking for and luminosity spheroid 19 inter- Correcting at of correct adopted redshift. procedure images and mediate the HST match scatter archival to intrinsic galaxies re-analyze active We time reverberation-mapped local first effects. substantially selection the is for for mass trends determine BH evolutionary in to range us covered allowing the increased, galaxies, Seyfert-1 40 totaling work, M http://arxiv.org/abs/0911.4232 BH th Yousuke Itoh, erpr u eeiaino h qain fmto o eaiitccom- relativistic for motion of equations the of rederivation our report We M shri uioiy( luminosity -spheroid rq;msiebnre fbakhls otNwointheory post-Newtonian holes; black of binaries massive gr-qc; BH ttlhs-aaylmnst eaini paetynneovn.It non-evolving. apparently is relation luminosity host-galaxy -total o tr itiueaon asv lc hole black massive a around distribute stars How M BH M / L BH L sph sph / L ∝ eain ncmiainwt u previous our with combination In relation. ) sph (1 ∝ + (1 z ) + M 2 . 8 z BH + a 1 2010 21, May ) / 1 − . .W td h omcevolution cosmic the study We ). 4 1 + . 2 / hnicuigasml of sample a including When . − 0 . 2 h nrni cte fthe of scatter intrinsic The .

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1. oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 Eprint: Authors: Hole Black Oscillating an from Formation Ring ubl .Shee . rmr . acaMrn . unrah . ui,K.; Muzic, Eprint: D.; A. Kunneriath, Zensus, M.; C.; Straubmeier, Garcia-Marin, N.; Sabha, M.; S.; Bremer, Nishiyama, R.; Schoedel R. suebel, of Importance Authors: A*: Sagittarius polarimetry infrared of near flares infrared Near s "kick", km a receiving 200 remnant merger order the in of result can mergers (BH) hole black Massive Abstract: Keywords: lc oea h aatcCne.Teosrain aebe are u sn the using out carried been have observations The Center. super-massive Galactic the the with at associated hole counterpart A*) black (Sgr A* Sagittarius the of vations Abstract: holes black Keywords: h ifrnilrtto fteds tece h aeit iglk segments. ring-like into wake the stretches disk the of the rotation as differential The well as where calculated wake is supersonic wake BH. a the the it of of behind shape time the The leaves slow-down to BH triggered. parallel be the motion may that BH formation find For star we kpc. 1 galaxy and the 0.2 of between plane near lie stars radii of resonant ring the to a that find of lead formation can the which trigger density may disk shock r and the there flow turn radii radial In resonant the formation. the of shock Near enhancement disk. strong the a of be plane radii" can the "resonant in frequency the epicyclic than resonant radial less strong the somewhat a dark but is near there isothermal motion that an r radial find and disk we the bulge, motion of con- perpendicular model forcing galaxy the Plummer model For a a for halo. disk, galaxy matter exponential the an of galaxy plane of the the through sisting to oscillates BH parallel the or where perpendicular case centre the analyze we Here centre. galaxy R R sa xml,fraB asof mass BH a for example, an As . hr h Hoclainfeunyi qa n-af n-orh 16 t. of etc.) (1/6, one-fourth, one-half, equal is frequency oscillation BH the where http://arxiv.org/abs/0911.4659 http://arxiv.org/abs/0911.4481 oeae .V . onec,D A. D. Kornreich, E.; V. R. Lovelace, erpr nterslso e iuain fna-nrrd(I)obser- (NIR) near-infrared of simulations new of results the on report We aaiaa,M;Ekr,A;Wte,G;Dvik . aa,V;Gies- V.; Karas, M.; Dovciak, G.; Witzel, A.; Eckart, M.; Zamaninasab, sr-hG;atohsc;kcsrci;sprasv lc holes black supermassive kicks/recoil; astrophysics; astro-ph.GA; sr-hG;atohsc;osrain;SgtaisA;supermassive A*; Sagittarius observations; astrophysics; astro-ph.GA; o tr itiueaon asv lc hole black massive a around distribute stars How − 1 rmr,wihwl as h enn ooclaeaotthe about oscillate to remnant the cause will which more, or 10 WNotes GW 8 M

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81 oe esfrG science GW for News & Notes Notes & News for GW science 82 WNotes GW ut rmftr bevtoso L nefrmtylk RVT xeietare experiment GRAVITY like discussed. is interferometry also VLT pattern re- of This Expected observations future noise. gravity. from red strong sults polarized a of randomly of against influence significant detection the statistically the under light detected in observed matter result and orbiting algorithm predicted of recognition of signature pattern comparison a a by through as predicted features well of also curve parameters as is polarimetric curves and correlation light intensity observed same between polarimet- the the Correlations in that model. changes spot confirm and hot we the curves Furthermore, light the density between data. flux correlation ric a observed Karas- of the the existence used of using the We probe out modulations We 2008). an carried code. of May been ray-tracing parts 28 have (KY) inner simulations and Yaqoob the relativistic 2007 in The May electrons 17 relativistic disk. from 2007, accretion emission May synchrotron 15 of 2006, 2004, model June June a (13 1 telescope Subaru 2005, Observatory’s the July Southern on 30 camera European NIR the CIAO and at Telescope Large instrument Very (AO) optics adaptive NACO ai.W ics h osblt fsprtn h fet fselrperturbations stellar of all effects at the problematic separating GR GR. of to of due possibility tests those the from make discuss would We region this requireradii. in to holes, likely black is moment Solar-mass quadrupole inside the stars are of of perturbations measurement beyond observation stellar stars while for that hole, frame-dragging black find to We the due signal the of considered. obscure distribution to are the likely for remnants models the stellar possible present of and We number stars A post-Newtonian out. effects. a carried include spin-orbit which be of simulations, region treatment such can this of simulations in set comprehensive stars N-body a of of full results number that expected enough The as small magnitude effects. of is relativistic order general same the to of due precession fromthat orbital perturbations induce of may presence which stars the stars, is of other factor complicating monitoring One "no-hair" astrometric relativistic 2008). (Will general via of theorems tests measured allowing distances, be (mpc) milliparsec principle at orbiting in can center Galactic Abstract: dynamics stellar A*; Sagittarius conjecture; Keywords: Eprint: Authors: Us- Orbits Hole Stellar Black ing Center Galactic the of Properties Testing http://arxiv.org/abs/0911.4718 ert,Dvd lxne,Tl ikl,Spo il lfodM. Clifford Will, Seppo; Mikkola, Tal; Alexander, David; Merritt, h pnadqarpl oeto h uemsiebakhl tthe at hole black supermassive the of moment quadrupole and spin The sr-hC;atop.A srpyis MI rq;Nbd;no-hair N-body; gr-qc; EMRI; astrophysics; astro-ph.GA; astro-ph.CO; o tr itiueaon asv lc hole black massive a around distribute stars How ∼ . p.Ahg rcino tla enns ..10- e.g. remnants, stellar of fraction high A mpc. 0.2 a 1 2010 21, May

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. p from mpc 0.5 oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 Abstract: Keywords: Eprint: Authors: Fields Magnetic Gamma- Strong of for Effects Bursts: Magnetars Ray around Disks Hyperaccreting Keywords: Eprint: Authors: inspi- in binaries effects compact tidal ralling of description Body One Effective aynurnsa ytm.Oraayi ugssteiprac fhigher-order to post-Newtonian tendency of first their the importance and beyond the order, even effects, suggests tidal analysis to to Our corrections formalism (post-Newtonian) systems. bi- tidal-EOB of star this sequences neutron of circular nary quasi-equilibrium prediction flat the nonconformally which compare formalism computed We (EOB) recently to body one up effects. effective (essentially tidal the inspiral de- of includes late analytically extension an of the propose hope during state we the phasing of contact) In wave equation gravitational nuclear parameters. the tidal the scribing relativistic on on information dependence crucial its yield via principle in can spirals Abstract: waveforms theory; Newtonian etgt h fet fsrn ed ntedssaon antr,addiscuss and magnetars, in- around We disks the process. accretion on funnel fields the strong to of lead effects even the and vestigate engines. properties central disk (GRB) the burst fecting gamma-ray of field candidate strong a The be can emission neutrino state of sufficiently equation a nuclear han- that the reliable hope on a the us dle raises give might but model model, EOB analytical numerical–relativity–“calibrated” the accurate late-inspiral of the choice of the insensitivity to strong of phasing the phasing shows comparison the This of systems. non- spiralling description advocated, (“Taylor-T4”) recently based some to post-Newtonian predictions EOB resummed, the compare We stars. neutron of http://arxiv.org/abs/0911.5528 http://arxiv.org/abs/0911.5041 hn,Dn;Di .G. Z. Dai, Dong; Zhang, Alessandro Nagar, Thibault; Damour, Arde)Tehprcrtn eto tro antrdsscoe via cooled disks magnetar or star neutron hyperaccreting The (Abridged) h aepr ftegaiainlwv inlo iaynurnsa in- star neutron binary of signal wave gravitational the of part late The sr-hH;atohsc;E counterparts EM astrophysics; astro-ph.HE; fetv n oy rq;msiebnre fbakhls post- holes; black of binaries massive gr-qc; body; one Effective o tr itiueaon asv lc hole black massive a around distribute stars How ≥ 10 15 − 10 16 significantly ftemgea a lyasgicn oei af- in role significant a play can magnetar the of G WNotes GW nraete“fetv ia polarizability” tidal “effective the increase

83 oe esfrG science GW for News & Notes Notes & News for GW science 84 WNotes GW ognrt n eda lr-eaiitcjtaogteselrmgei poles. magnetic stellar the along jet together ultra-relativistic work an can and feed surface and mechanism magnetar generate annihilation the to from neutrino wind the pulsar Furthermore, neu- magnetically-driven accreting the from fields. that than without higher stars annihilation much be neutrino tron can the magnetar magnetars accretion, accreting the the funnel from Because of by rate covered emission disk. region neutrino belt plane concentrated ring-like the more surface truncates and and temperature funnel radius higher The Alfvén createsof which the stress. field, inside strong viscous extremely magnetosphere an the for a than important only disk be transferring the will in process heating role accretion important and the more momentum near a unstable angular plays thermally field the be magnetic the will where but radius radius, Alfvén Alfvén the always is outside disk stable magnetized A viscously significantly. state degeneracy change and and fraction luminosity, electron give neutrino the fields and stronger temperatures general, pressures, In scale densities, large interaction. disk conser- a star-disk higher MHD with the coupled by the flow generated use disk is and the which of disk, field, behavior the the on describe to fields We equations strong events. vation the GRB-like of and effects GRB quantum for systems discuss magnetar accreting such of implications oagetteeetoantcrdainoe ogrtimescales. combine longer can sources over heat radiation two electromagnetic these the adjust- radiation; augment orbital gravitational to from in lost gained of mass energy orientation the the spin to of new ment dissipation the supplement can to hole orbits mass, black distances, gas gas the larger the the somewhat realigning to At with proportional event. associated is merger the signal dissipation than photon longer the rather independent of generally luminosity is duration and Eddington The the emit- mass. is luminosity gas merger the the the of of with scale association amount characteristic direct small) the in surface (quite thick, the ted the optically than and it greater mass, is make total vicinity to its immediate necessary the to in proportional gas is the holes of gas black density the merging in of deposited heat pair the a whenever immediate near that in show We occur might events. that these with luminosity conjunction electromagnetic very the mergers, about hole black known of is luminosity little wave gravitational the quantifying in strides Abstract: Keywords: Eprint: Authors: Merger a Hole of Black Luminosity Electromagnetic Prompt the Estimating http://arxiv.org/abs/0911.5711 rlk uinH. Julian Krolik, lhuhrcn oki ueia eaiiyhsmd tremendous made has relativity numerical in work recent Although sr-hC;atop.E srpyis Mcounterparts EM astrophysics; astro-ph.HE; astro-ph.CO; o tr itiueaon asv lc hole black massive a around distribute stars How

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 oeeti h tkspae eitrrtteeeet sasokfotmoving front shock a as events these underly- interpret an We circular a from plane. exhibits emission Stokes sometimes as emission the explained jet in chaotic be movement is The can core component. and polarization jet years quiescent optical of ing The scales an time emission. components: on jet two stable chaotic posi- into and emission preferred jet core The the polarization separating polarization. optical by explained optical be in can angle angle We tion position vari- light-curve. preferred analyse polarization strong to optical aim a the we of find firstly, properties twofold: statistical is and study patterns this ability double-peaked of latest aim the The which occurred. during outburst 2005-2009, from data monitoring larimetric Eprint: Authors: perturbations hole black of Asymptotics Keywords: N. Bergvall, A.; Eprint: Aungwerojwit, S.; Li- Haque, C.; C.; W. J. Coggins-Hill, Yee, Keel, D.; Marchev, L.; A.; Mattingly, Watson, A.; Donmez, A.; J.; S.; S. Prieto, W.; Dogru, S.; D. K.; Gazeas, M. Atlee, P.; Peeples, Niarchos, J.; A.; J.; R. akos, Eastman, Assef, L.; M.; Kamada, D. Dietrich, K.; DePoy, M.; J.; Sadakane, A.; Nissinen, Y.; Bird, -P.; Efimov, V. Kuzmicz, X.; Hentunen, Zhou, C.; J.; -H.; Ohlert, Porowski, J. M.; Kurpinska- Wu, W.; D.; T.; Ogloza, Kundera, Koziel-Wierzbowska, J.; M.; M.; Krzesinski, Drozdz, Siwak, M.; Winiarski, M.; M.; Winiarska, Pasanen, E.; Lindfors, A.; Authors: 2005- in of 2009 OJ287 scales of time monitoring polarization on Optical jets years: blazar in stability and Variability wide a in theory. perturbation helpful hole be black employing should applications of approach of studies hyperboloidal range in domain The impor- computational the the radiation. stress in gravitational We region asymptotic the coordinate. including radial of hy- compactifying tance using a domain and time surfaces in perboloidal equations Regge-Wheeler-Zerilli numerically solving by Abstract: Keywords: trglritrasof intervals regular at Abstract: http://arxiv.org/abs/0912.0005 http://arxiv.org/abs/0911.2450 egngu Anil Zenginoglu, ilot,C;Nlsn . ed,J;Tkl,L . usm,T;Berdyugin, T.; Pursimo, O.; L. Takalo, J.; Heidt, K.; Nilsson, C.; Villforth, Arde)O27i LLcojc hthssondul-ekdbursts double-peaked shown has that object Lac BL a is OJ287 (Abridged) esuylna rvttoa etrain fShazcidspacetime Schwarzschild of perturbations gravitational linear study We sr-hC;atohsc;msiebnre fbakhls observations holes; black of binaries massive astrophysics; astro-ph.CO; rq;lnaie hoy ueia ehd;nmrclrelativity numerical methods; numerical theory; linearized gr-qc; o tr itiueaon asv lc hole black massive a around distribute stars How ∼ 2y uigtelast the during yr 12 WNotes GW ∼ 0y.W nls pia photopo- optical analyse We yr. 40

85 oe esfrG science GW for News & Notes Notes & News for GW science 86 WNotes GW edlns mgei rahn’o h disc. magnetic the of of accretion breathing’ polar- resonant ’magnetic optical of a sign the lines, a of as field explained evolution We be the could and OJ287. angle position bursts understanding ization double-peaked to the approach both new pos- that a discuss We suggest propose observations. and all explain explanations to re- new able and and sible is list models mass this the using hole of models none black existing that the all conclude rate as We properties. such flow the OJ287, accretion of on of characteristics strictions properties only not other to includes also list list proposed but The a models light-curve fulfil. compose to We hole has OJ287. black model a in binary requirements bursts Sec- of different double-peaked assess field. appearing regularly magnetic to the helical data explain a our through use swiping we jet, ondly, the in backwards and forwards xml h iigmthfitrn eoe pia nyi h N slre than larger is SNR spectrum. the wave if gravitational the only For of optimal kurtosis errors. becomes the estimation filtering insight and match new timing SNR provides the the properties and example correctly waveform CRLB predicts between the relationship also with the It error on the simulations. approximate numerical to predictions in error SNR get observed necessary to is allows The what expansions variance to estimates. the closer of numerical We order existing second . with the interferometers estimate of wave value error gravitational improved of the inspiral noises compare the for from also parameters and physical mergers of sec- binary MLE the of for first compute bias phase the we can and application where variance estimate an ratios the As MLE of noise CRLB. order a the to ond is of signal expansion bias the variance the of the in to powers and order signal inverse variance large in the for instead how errors expressed here the be show approximate We to mean ratios. a Cramer noise the as of (CRLB) usage the bounds on Lower focuses litterature Rao Grav- existing from the parameters All physical signals. for wave (MLE) itational estimate likelihood maximum a for error Abstract: gorithms Keywords: Eprint: mergers Authors: waves binary of gravitational phase to inspiral the application in generated an with errors, tors estima- Likelihood Maximum of expansions Asymptotic http://arxiv.org/abs/0912.0065 aoi,M;Vtl,S;Mki,N. Makris, S.; Vitale, M.; Zanolin, nti ae edsrb e ehdlg ocluaeaayial the analytically calculate to methodology new a describe we paper this In rq;msiebnre fbakhls aaee siain erhal- search estimation; parameter holes; black of binaries massive gr-qc; o tr itiueaon asv lc hole black massive a around distribute stars How

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 eaiitcMreso uemsieBakHlsand Holes Signatures Electromagnetic Black their Supermassive of Mergers Relativistic pnigcmatbnr nprl needn vari- configurations spin Independent preserved dynamically and inspiral: ables binary compact Spinning Abstract: relativity numerical holes; black of ries Keywords: Authors: Keywords: Eprint: Authors: Eprint: Deirdre maker, asssesadbnre mesdi o est min a a nyb de- be only can gas ambient density universe. lower local low while the 1, in in = immersed tected z to binaries most searches and the EM by systems of identified case mass be calculated the may Antenna, they In Space that Interferometer imply counterparts. Laser luminosities EM the for by searches observable signa- binaries in characteristic holes massive some utilized black exhibit be orbiting systems can all where but that and wakes, tures axis density of sys- orbital set for the stable observed with a the is form aligned with variability are combined EM spins striking accretion where most and arise tems The can shocks GWs beaming. of with relativistic consequence correlated of a signatures effect EM as variable systems that binaries merging find hole in We black cloud. supermassive gas spinning we a the equal-mass, in goal, of of study this merger hydrodynamical and towards relativistic, inspiral step general late fully essential first an mergers the As hole from results black present importance. supermassive paramount during of arise therefore signatures coin- is GW which and under cosmological EM conditions independent of the provide cidences Understanding will precision. and high rela- regime to general nonlinear measurements testing strong, enable the will in observations gargantuan study tivity the these to generally, with More means associated the objects. processes compact provide accretion will and next detections the evolution Such are cosmological holes black challenge. supermassive grand of observational events coalescence from signatures (GW) http://arxiv.org/abs/0912.0087 http://arxiv.org/abs/0912.0459 egl,Lsl Árpád László Gergely, oe aj;Ha,Rln;Bgaoi,Tmr;Lgn,Pbo Shoe- Pablo; Laguna, Tamara; Bogdanovic, Roland; Haas, Tanja; Bode, onietdtcin feetoantc(M n rvttoa wave gravitational and (EM) electromagnetic of detections Coincident rq;msiebnre fbakhls otNwointer;spin theory; post-Newtonian holes; black of binaries massive gr-qc; sr-hC;E oneprs eea eaiiy rq;msiebina- massive gr-qc; relativity; general counterparts; EM astro-ph.CO; o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW

87 oe esfrG science GW for News & Notes Notes & News for GW science 88 WNotes GW in,ee ntoeicuigol h atobt fteinspiral. the of orbits last the only evolu- including binary particular those compact in what of even on investigations tions, numerical limitations in severe selected puts be quadrupole- oriented can result configurations identically analytic and and This equal spin-spin mass, configuration. with equal spin the evolution is included post-Newtonian contributions the monopole which the configuration by that binary prove star preserved We neutron or is variables. hole these ana- black of spinning we and terms precessing mass Then in only and dynamics ap- spin orbits. spin conservative Our including nonspherical) the order, (noncircular, lyze post-Newtonian generic inspiral. second for the the effects, during to quadrupolar binary up compact valid is spinning proach the of evolution plicated Abstract: Eprint: With Authors: Binaries Diagnosis Hole Line Emission Broad Black Supermassive Identifying these of tests observational possible and epochs, that cosmic holes early black scenarios. at ‘seed’ place for processes to hole formation of black likely hole massive are some black the here of discuss review evolution will the I briefly to population. I conducive buildup are the that wells? await processes potential same physical to deeper the the had with with formation form galaxies their seeds was substantial did MBH it of or when Did proto-galaxies, stage hierarchical small components. the In in smaller to efficiency back of start? traced hundreds all be in it can up did today split galaxy When big structure. single galactic a cosmologies, of ( host evolution re- the These the than massive to dispersion. less velocity linked much and while MBHs, mass central bulge that and as suggest mass such sults MBH galaxy the between host relations the of of number properties a established also have Studies ies. Abstract: Keywords: Eprint: Authors: holes black massive of evolution early The http://arxiv.org/abs/0912.0541 http://arxiv.org/abs/0912.0525 hn u;Le,Abraham Loeb, Yue; Shen, Marta Volonteri, eetbihtesto needn aibe utbet oio h com- the monitor to suitable variables independent of set the establish We asv lc oe r oaasblee orsd nms oa galax- local most in reside to believed nowadays are holes black Massive sr-hC;atop.E omlg;sprasv lc holes black supermassive cosmology; astro-ph.HE; astro-ph.CO; o tr itiueaon asv lc hole black massive a around distribute stars How a 1 2010 21, May

∼

.%,are 0.1%), oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 aySBsadhglgttedfeetbhvoso eebrto apn nthe in mapping scenarios. bi- reverberation emitter for of disk profile behaviors and two line different binary broad the the the in profile highlight of and drifts line variations SMBHs velocity the temporal nary the radial distinct, discuss coherent longer We no no time. are with are peaks there BLRs and two complex the more two that the becomes such when However, closer when components. even difference broad motion are velocity individual orbital BHs orbital of binary light-of-sight FWHM the the the that than to larger such due is enough close peaks are two BLR BHs the features two the of the double-peaked at of drifts flux emergence ionizing velocity the the radial confirm that and we and constant, (BHs) roughly holes is BLRs black position both two sep- that the various assumptions by with reasonable illuminated binary Under are SMBH models. emission. a BLR line for simple the profiles using for line arations, origin broad disk interpre- expected a alternative the is broad An feature calculate We line two profile. broad whose line double-peaked binary the the of to (SMBH) tation together hole contribute black (BLRs) supermassive regions a line of existence the cate Abstract: holes Keywords: eoeyo inl rmcipn aatcbnre,fo pnigsupermassive– spinning between from SNRs optimal binaries, positive (with the Galactic binaries demonstrated chirping black-hole which from 2008, signals Apr of in issued the recovery present challenge, we third Here the the parameters. analyze of source results the Participants for grav- solutions parameters. best-fit and report undisclosed noise and of datasets instrument sources simulated from containing waves datasets itational more challenges or of round one Each of development. consists their encourage to and capabilities analysis Abstract: Keywords: Eprint: Whelan, John; Veitch, Miquel; Andrzej; Trias, T. Yu; Królak, John Shang, Shapiro; Farhan; Reinhard; Joey Key, Prix, Feroz, Mike; Anthony; Curt; Hobson, Lasenby, A.; Cutler, Philip; Keith Graff, Michael; R.; Arnaud, Cohen, Jonathan Matt; Gair, Michael; Adams, Bridges, Robinson, Alberto; Arkadiusz; K.; Vecchio, Edward Błaut, Porter, Michele; Antoine; Vallisneri, Petiteau, L.; Ilya; Emma Mandel, L.; Shane Larson, J.; to Authors: 3 Challenge from 4 Challenges: Challenge Data LISA Mock The http://arxiv.org/abs/0912.0548 h okLS aaCalne r rga odmntaeLS data- LISA demonstrate to program a are Challenges Data LISA Mock The aa,Sailv ae,Jh . eaqit,MthwJ;Crih Neil Cornish, J.; Matthew Benacquista, G.; John Baker, Stanislav; Babak, obepae ra ie nAtv aatcNce AN)myindi- may (AGNs) Nuclei Galactic Active in lines broad Double-peaked rq;MLDC gr-qc; sr-hC;atohsc;E oneprs asv iaiso black of binaries massive counterparts; EM astrophysics; astro-ph.CO; o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW ∼ 0ad20) rmsimultaneous from 2000), and 10

89 oe esfrG science GW for News & Notes Notes & News for GW science 90 WNotes GW Eprint: for Authors: estimation parameter binaries LISA hole black on nonspinning mergers of Impact with background noise. isotropic instrument loud LISA the relatively below a slightly from and (SNRs 10-100), bursts cosmic-string-cusp of from 10-50), of (SNRs inspirals extreme-mass-ratio Keywords: Eprint: Holes Authors: Black Around Flow Accretion Sub-Keplerian a in Waves Shock Oscillating of Simulations Hydrodynamic arcmin). O(1 within to localized can be half can 10% investigation, and under arcmin), systems O(10 within precise to most localized the increase be the For to ratio. comparable is signal-to-noise For merger in the observation. mass including of from total resulting minutes precision final with creased sky- the systems in even improvements and mass significant hours comparable last to the lead in signal precision real-time the In position of merger. parts pre- the later the of the to inclusion observations, content from and higher-order resulting formalism, and uncertainties matrix parameter asymmetry dicted mass Fisher of the significance using the uncertainties establish parameter masses the total and compare 1/10, wave- We >= nonspinning q covers ratios, analysis mass Our moderate with ringdown. that merg- forms and nonspinning find merger for we the estimates ignored previous signals, that than the ers precision of greater far portions have ringdown will measured and LISA merger be waveforms complete inspiral, can using the By binaries (LISA). including Antenna hole Space black Interferometer Laser nonspinning the with of location and characteristics Abstract: Metropolis-Hastings holes; black of binaries massive interferometers; Keywords: http://arxiv.org/abs/0912.1174 http://arxiv.org/abs/0911.1078 cilas enT;Top,JmsIa ae,Jh . el,BradJ. Bernard Kelly, G.; John Baker, Ira; James Thorpe, T.; Sean McWilliams, ii isk hkaat,Sni . aat,MdnM;Ru Dongsu Ryu, M.; Madan Samanta, K.; Sandip Chakrabarti, Kinsuk; Giri, eivsiaetepeiinwt hc h aaeesdsrbn the describing parameters the which with precision the investigate We crto ic;atop.E Mcounterparts EM astro-ph.HE; discs; accretion srpyis aaaayi;E oneprs eea eaiiy gr-qc; relativity; general counterparts; EM analysis; data astrophysics; o tr itiueaon asv lc hole black massive a around distribute stars How M / M a 1 2010 21, May

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7 , . oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 in oteeutoso oinalwu ocntante‘ohi’prmtrt be precision. to achievable parameter the ‘no-hair’ within the theorem’ constrain to us allow motion 1 of equations the to tions candidates. hole have black will of behaviours properties These timing made. and oppo- is spectral shock The the inner frequency. in the higher implications of higher the analysis indicates the at when location power true shock lower is and outer site frequency the lower of oscilla- the variation harmonic at the coupled power discontinuities of a two analysis as Fourier The behave A (d) and tor. role frequencies major different discontinuities. a the two these plays in with Turbulence of oscillate discontinuities point. locations two sonic the are inner determining There the of in (b) outside several just is scale. region being time post-shock one free-fall flow, the in the scale than time higher infall equilibrium The times vertical (c) with region. flow a post-shock and con- the region a in pre-shock to the close in behaves flow flow model dependent height time stant We The (a) considerations. results important theoretical the several compare from found and parameter obtained momentum the those angular scan with We the solutions and purpose. time-dependent energy this specific for the code by difference spanned finite space based grid a use We Abstract: Keywords: Eprint: R. Hudec, M.; Basta, R.; Saunders, H.; Rampadarath, T.; Hyvönen, OJ287 in hole Authors: black primary the of spin the Measuring uealtekonotuss nldn el icvrdoei 97 h Kerr the 1957, in be one to repro- discovered has to newly primary order a the In of including value. parameter spin outbursts, the known to reproduced. the sensitive is all quite 2007 duce are to outbursts up evalu- 1913 the are from of primary outbursts timings the times observed The of of specific record disk the the accretion solution, that the orbital such depends crosses the ated it secondary Using the expected of as hole. orbit and black the calculated primary when is the OJ287 of in spin terms, hole the spin-orbit black on binary classical the and of relativistic orbit general the order non-spinning Using primary accurate leading hole. 2.5PN spinning the black include a that contributions, secondary equations non-spinning contain accurate a to (PN) and Newtonian modelled disk Post accretion is an OJ287 with hole in black system binary compact The Abstract: spin observations; . 0 ± 0 http://arxiv.org/abs/0912.1209 . 3 esuyteaceinpoesso lc oeb ueia simulation. numerical by hole black a on processes accretion the study We atnn .J;Mkoa . ert,D;Gpkmr . et,H J.; H. Lehto, A.; Gopakumar, D.; Merritt, S.; Mikkola, J.; M. Valtonen, hr . steoesgaerr hsspot h bakhl no-hair hole ‘black the supports This error. sigma one the is 0.3 where sr-hC;atop.E srpyis asv iaiso lc holes; black of binaries massive astrophysics; astro-ph.HE; astro-ph.CO; o tr itiueaon asv lc hole black massive a around distribute stars How 0 . 28 WNotes GW ± 0 . 08 h uduoemmn contribu- quadrupole-moment The .

91 oe esfrG science GW for News & Notes Notes & News for GW science 92 WNotes GW eeto fIBsfo irlnigi lblrclus- globular ters in microlensing from IMBHs of Detection is spin the if 2016 is January of spin end the early the if in in starts begins spin: 0.2 event outburst the same the of relativity, the general function while is in 2015, strong outburst November allowed a next value is the maximal outburst when the 2015 2015 of the in 0.36 of estimate timing present The the test due. to possible be should It iebnre fbakholes black of binaries sive Keywords: Eprint: Authors: Mergers Massive Hole of Black Afterglows the for Models Time-Dependent of telescope. detectability class the 2-m discuss a and using duration strategy events time observational microlensing average the the present We estimate mi- and events. BH GCs the central Galactic of to of depth list optical selected the a for calculate We crolensing differential applied. the lens- be unresolved, the can if of technique possible; the determination are imaging direct by new parameters the stars system a resolved, cluster lensing is propose and the cluster curve we of the ing microlensing Here of core the the cores. – If BH GC BH. central central the the in of observational stars detection enormous search of of present in method crowding and attempts direct the the not to are of due (BHs) Most difﬁculties holes black relations. extrapolation, central same in the the that, of the follow suggest between do (GCs) correlations in galaxies clusters well-established host IMBHs globular their The host and may holes do. black clusters galaxies supermassive globular like their just galactic have in centres, evidence many them observational their that retain and and believe theoretical form enough to decade to accumulated last impossible the nearly Over or centres. (IMBHs) holes black mass Abstract: Keywords: Eprint: Authors: http://arxiv.org/abs/0912.2054 http://arxiv.org/abs/0912.1435 aaa aais;Mnu Kristen Menou, Takamitsu; Tanaka, S. C. Stalin, M.; Safonova, lblrcutr aebe lentvl rdce ohs intermediate- host to predicted alternatively been have clusters Globular crto ic;atop.O srpyis Mcutrat;g-c mas- gr-qc; counterparts; EM astrophysics; astro-ph.CO; discs; accretion sr-hG;atohsc;itreit-asbakhls observations holes; black intermediate-mass astrophysics; astro-ph.GA; o tr itiueaon asv lc hole black massive a around distribute stars How

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 aesgasfo olsigpiso asv lc oe ntettlms range mass total the in holes black massive of (10 pairs coalescing from signals wave Abstract: vr u iuain r nbet ombakhlswt assabove masses with holes black How- form . to reproduced unable adequately are is seeds simulations indi- of quasars, our history of ever, accretion simulations function average present luminosity the the bolometric that from the cating from derived derived density that mass Moreover, with hole mass. agrees halo black dark the our host of and z=0, evolution dispersion At the velocity black stellar the of with episodes. correlations both the merger nu- mass and hole a from function mass from resulting hole matter black coalescences the accreting reproduce by by simulations also essentially grow and Seeds disk present peaks clear 12-15. density into range inserted redshift masses the solar 100 in of simulations. seeds from cosmological grow through holes investigated Black are galaxies host their of properties Abstract: Keywords: Eprint: Authors: Simulations ical Cosmolog- from Holes Black Supermassive of Evolution n h mrec fotosaon asv lc oe ihpeieyknown precisely with holes black orientations. massive and around spins masses, outflows of flows emergence accretion for the of opportunities evolution and viscous unique the offer timescales LISA tractable by humanly that on detected monitoring conclude holes We black outflow. massive powerful of advec- a mergers become generate the could and flow the inefficient, innermost to radiatively the close and that tive thick indicating circumbinary evolves, geometrically innermost it increasingly as the becomes object also by We central disk frequencies. X-ray spreading infrared the and soft optical that the at reprocessed find in partially be emitted may is it Ed- but It local disk, the limit. violating The flux without thought. luminosities dington previously super-Eddington than brightening earlier reach years rapidly can several a afterglow i.e. merger, as the observable after that soon become suggest source may calculations corresponding Our counterpart the electromagnetic and disk. an evolution circumbinary func- the viscous Green’s of temporal using signature by the electromagnetic scenario calculate this to revisit We solutions tion event. wave gravitational the after ei hne 20)pooe htacrubnr ikaon iayo mass of binary a around disk circumbinary a that ∼ proposed (2005) Milosavl- Phinney holes. & black massive jevic offer well-characterized and around physics studies gas cosmological of enable probes new would events these of counterparts magnetic 10 5 − 6 M 10

http://arxiv.org/abs/0912.2223 7 ) ilei naceinpwrdXryatrlwapoiaeyoedecade one approximately afterglow X-ray accretion-powered an emit will / ilu,C. uir . ahc,J .d ria;Sl,J. Silk, Freitas; de A. J. Pacheco, F.; Durier, Ch.; Filloux, h ae nefrmtrSaeAtna(IA ildtc gravitational detect will (LISA) Antenna Space Interferometer Laser The M h orltosbtentems fsprasv lc oe and holes black supermassive of mass the between correlations The sr-hC;csooy uemsiebakholes black supermassive cosmology; astro-ph.CO;

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93 oe esfrG science GW for News & Notes Notes & News for GW science 94 WNotes GW Eprint: Authors: Ac- cretion Bondi-Hoyle-Lyttleton" Environments: "Binary Gaseous and Bondi" in "Binary Mergers Hole Black Binary range. redshift this in survey z nacmnsi ohteaceinrt n uioiyoe ausfrasingle a a enhance- for luminosity n LSST for this by that values detectable estimate We be over binary. should the luminosity ment as mass and same the rate of accretion hole significant black for luminosity the evidence electromagnetic both find the We in estimate emission. enhancements and synchrotron and rate bremsstrahlung accretion to and due flow a gas gas by the governed The and vary pute We binary cloud. the gas state. from the of far Bondi-Hoyle- homogeneous equation to "binary be as relative to well moves assumed as binary is cloud, cloud the gas which ambient in the the accretion" to which Lyttleton relative in rest accretion" at Bondi punc- "binary is shock- moving both binary high-resolution consider standard a We via with scheme. hydrodynamics (HRSC) formulation the capturing handle BSSN and the conditions gauge using ture metric clouds. the gas in evolve embedded simula- We binaries BHBH hydrodynamic nonspinning relativistic, equal-mass, general merging, of fully tions performing inves- by We cosmology. scenario and this physics, tigate oppor- accretion of physics, the wealth gravitational a in study provide enhancements to can tunities and detection simultaneous variability a produce Such shock may flux. stirring, gas electromagnetic the the as of simultane- accretion radiation, a and of gravitational possibility heating and a electromagnetic is of there such environment, If detection gaseous ous a waves. in gravitational place detectable takes of merger sources a promising are mergers galaxy in Abstract: relativity numerical holes; black of binaries sive Keywords: r/,wt h msinpaigi h iil band. visible the in peaking emission the with erg/s, ∼ ∼ 10 6 hs xsec sifre rmtebih usr eetdb h Sloan the by detected quasars bright the from inferred is existence whose , / cm http://arxiv.org/abs/0912.2096 ars ra . i,YkTn;Saio tatL. Stuart Shapiro, Tung; Yuk Liu, D.; Brian Farris, 3 egn uemsiebakhl-lc oe(HH iaisproduced binaries (BHBH) hole hole-black black supermassive Merging n eprtr T temperature and crto ic;atop.E srpyis Mcutrat;g-c mas- gr-qc; counterparts; EM astrophysics; astro-ph.HE; discs; accretion o tr itiueaon asv lc hole black massive a around distribute stars How Γ ewe / n /.Frec iuain ecom- we simulation, each For 5/3. and 4/3 between ∼ 10 6 tz1 ecigamxmmo L of maximum a reaching z=1, at K 10 6 M

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43 oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 iln h ikhlo olwn iaybakhole black binary afterglow following accretion transient The hollow merger: disk the Filling Eprint: mergers Authors: waves binary of gravitational phase to inspiral the application in generated an with errors, tors estima- Likelihood Maximum of expansions Asymptotic Keywords: Eprint: Authors: gorithms Keywords: oqe n icst ananteinreg fteds tardu r radius a tidal at between disk the balance of The edge inner the disk. maintain accretion viscosity gaseous and torques circumbinary any in regions Abstract: holes black of binaries massive gr-qc; parts; infaue n clnsta hrceieti rnin.I a ev sagiein simulations guide radiation-magnetohydrodynamic a relativity. as future general serve of in can calibration It highly and emis- transient. design thermal though this parameters, characterize the model, key that Our the scalings of and some features decoupling. establishing sion to in rate prior useful the be Eddington if may below phase initial idealized, secular far the a this very of during by not existence accretion detected is super-Eddington very merger to the BHBH lead how a can show confirm hollow We help may the interferometer. of fills wave hardening hole gravitational the donut and flux the electromagnetic as total Observ- spectrum the in radia- epoch. increase accretion electromagnetic temporal to transient the the this relaxes ing calculate during then to emitted and model spectrum orbit the ("afterglow") our circular up tion use stable fills We it innermost as hole equilibrium. disk black stationary the the of to evolution disk down (viscous) Newtonian the hollow secular time-dependent, in the simple, hole") a follows ("donut present that We hollow calculation hole. central black a decouples remnant behind binary the leaving inspiraling orbiting the merges, Eventually, and axis. disk semimajor from binary the is a where http://arxiv.org/abs/0912.2345 http://arxiv.org/abs/0912.0065 aoi,M;Vtl,S;Mki,N. Makris, S.; Vitale, M.; Zanolin, L. Stuart Shapiro, ia oqe rmabnr lc oe(HH mt u h central the out empty (BHBH) hole black binary a from torques Tidal rq;msiebnre fbakhls aaee siain erhal- search estimation; parameter holes; black of binaries massive gr-qc; crto ic;atop.O sr-hH;atohsc;E counter- EM astrophysics; astro-ph.HE; astro-ph.CO; discs; accretion o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW ∼ .a–2a, – 1.5a

95 oe esfrG science GW for News & Notes Notes & News for GW science 96 WNotes GW xml h iigmthfitrn eoe pia nyi h N slre than larger is SNR spectrum. the wave if gravitational the only For of optimal kurtosis errors. becomes the estimation filtering insight and match new timing SNR provides the the properties and example correctly waveform CRLB predicts between the relationship also with the It error on the simulations. approximate numerical to predictions in error SNR get observed necessary to is allows The what expansions variance to estimates. the closer of numerical We order existing second . with the interferometers estimate of wave value error gravitational improved of the inspiral noises compare the for from also parameters and physical mergers of sec- binary MLE the of for first compute bias phase the we can and application where variance estimate an ratios the As MLE of noise CRLB. order a the to ond is of signal expansion bias the variance the of the in to powers and order signal inverse variance large in the for instead how errors expressed here the be show approximate We to mean ratios. a Cramer noise the as of (CRLB) usage the bounds on Lower focuses litterature Rao Grav- existing from the parameters All physical signals. for wave (MLE) itational estimate likelihood maximum a for error Abstract: aeojcsi otglxe fsmlrms nteLclUniverse. Local the extremely in mass become similar high-redshift, of at galaxies most host phase that in quasar propose objects We their rare luminosity. living quasar holes, the black of and massive loudness radio the of the gardless that find factor we a population, by redshift stellar increases sampled the the of in aging that, the show count We age. Universe the the of range, cent per 85 along lation Abstract: holes black Keywords: Eprint: age present the Authors: to z=3 from evolution for Evidence - quasar The ihti aaw r bet i onterdhf eedneo the of dependence redshift the luminosities. down pin their to from able inferred are were re- we masses data line galaxy this known. broad With host are the the which in while of equilibrium I), luminosities virial (Paper galaxy assuming gions host estimated the were quasars masses 96 hole of Black sample a for z=3 to http://arxiv.org/abs/0911.2988 eal,R;Flm,R;Tee,A;Lbt,M;Ktlie,J . cra R. Scarpa, K.; J. Kotilainen, M.; Labita, A.; Treves, R.; Falomo, R.; Decarli, nti ae edsrb e ehdlg ocluaeaayial the analytically calculate to methodology new a describe we paper this In esuytedpnec fthe of dependence the study We M sr-hC;atop.A srpyis omlg;supermassive cosmology; astrophysics; astro-ph.GA; astro-ph.CO; bh − o tr itiueaon asv lc hole black massive a around distribute stars How M L host bh ∼ eainrmisnal nhne.Oc etk noac- into take we Once unchanged. nearly remains relation rmz0t =.W hwta am vle ihzre- z with evolves Gamma that show We z=3. to z=0 from 7 − M host eaintruhCsi ieII Time Cosmic through relation M bh a 1 2010 21, May − M host eaino h esitup redshift the on relation M bh / M host ai (Gamma) ratio M bh − M host

re- oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 aae n lc oemasses hole black and Dataset quasar The h e,wihi unrflcsta h ula ein fteB a bet aea have objects Lac BL the of regions Flat nuclear than the of luminous that power reflects low the turn to relatively linked in are be which Lacs might jet, BL luminosity the The that (FSRQs). observed originated Quasars is be and Radio to It Spectrum Lacs believed (BL are blazars jets. emission of their their case of from In most Quasars), proportional object. Radio a central Spectrum has the Flat jets of astrophysical spin observed black the the the the with that of of correspondence spin power shows the the clearly with that model strongly inferring The increases hole, disk holes. the black from extracted the power rota- of on outflow depend spin the strongly and on disk-outflow rate of dependence energetics accretion strong The mass, hole. its black and the of surface parameter investigate disk-outflow tion We the laws. of conservation properties the upholds the essentially accretion and dynamics Inter-connecting outflow of flux. vertical cou- the disk-outflow and explicitly advective incorporating accretion an dynamics, model pled that we Here, reveal correlated. insights strongly are theoretical outflow/jet deeper several and Notwithstanding, evidences elusive. observationally observational remains still systems, hole black Abstract: holes black permassive Keywords: Eprint: brata Authors: holes black spinning around Energetics coupling: Disk-outflow Abstract: Keywords: Eprint: Authors: lc oems n h otglx uioiyadms nCsi Time. Cosmic on mass and the luminosity between galaxy ratio host the the of and dependence mass the hole address black how we paper, illustrate companion then a sample, We In the cedure. describe observations. we spectroscopic paper new derive this the we In and epoch. sources present the data to the z=3 from quasars 96 of http://arxiv.org/abs/0911.3049 http://arxiv.org/abs/0911.2983 eal,R;Flm,R;Tee,A;Ktlie,J . aia . cra R. Scarpa, M.; Labita, K.; J. Kotilainen, A.; Treves, R.; Falomo, R.; Decarli, esuythe study We htahra ebjy hs,Suhagh;Mkoaha,Bani- Mukhopadhyay, Shubhrangshu; Ghosh, Debbijoy; Bhattacharya, M h ehns ywihotosadpasbejt r rvnfrom driven are jets plausible and outflows which by mechanism The sr-hC;atohsc;csooy uemsiebakholes black supermassive cosmology; astrophysics; astro-ph.CO; crto ic;atop.E srpyis Mcutrat;si;su- spin; counterparts; EM astrophysics; astro-ph.HE; discs; accretion bh rmsnl-pc pcr,pitn u h netite ntepro- the in uncertainties the out pointing spectra, single-epoch from o tr itiueaon asv lc hole black massive a around distribute stars How M bh M − bh M − M host host eaintruhCsi ieI- I Time Cosmic through relation eaina ucino omcTm nasample a in Time Cosmic of function a as relation WNotes GW

97 oe esfrG science GW for News & Notes Notes & News for GW science 98 WNotes GW Eprint: Authors: dwarf white galactic binaries the for Challenge Data LISA Mock as- observed system. the powered for black accretion account the an ex- of to in spin parameter the processes then trophysical fundamental If jets, the FSRQ. and be of outflows might strong case perhaps, power the hole, to in source that the is to gravity compared treme hole black spinning low relatively lc oe htpwrterdoeitn esi hs ore.Uiggnrlrela- central general the Using axisymmetric of state sources. inves- steady spin these We construct the in we simulations, jets in 1000. magnetohydrodynamic radio-emitting differences of tivistic the to factor power due a that be by holes can AGN black dichotomy quiet radio this similar whether of tigate power the exceeds age Abstract: Keywords: Eprint: Authors: Dichotomy Nuclei Loud/Quiet Galactic Radio Active of the and Spin Hole Black sig- thousand ten We than binaries. procedure. more dwarf the of white repeat from accurately nals we parameters al- and Nelder-Mead estimate the found and using reliably signal parameters strongest detect bank refine the we template remove then the search, we through the gorithm, data of the step max- first filter the the We strongly is at procedure is method. analysis signals data detection basic the likelihood Our between imum mHz. confusion 5 above The frequen- frequencies low at individually. at reduced resolved signals the not to of are added Majority were cies noise. binaries instrumental Galactic the where Gaussian mln. 3.1, simulated 50 Challenge the than of more analysis from the signals on wave is Mock gravitational focus the main in Our binaries dwarf Challenge. white Data the LISA from signals wave gravitational of parameters Abstract: Keywords: http://arxiv.org/abs/0911.2228 http://arxiv.org/abs/0911.3020 łu,Akduz aa,Sailv rlk Andrzej Królak, Stanislav; Babak, Arkadiusz; Błaut, cehvky lxne;Nryn aeh ciny oahnC. Jonathan McKinney, Ramesh; Narayan, Alexander; Tchekhovskoy, epeetdt nlssmtosue ndtcinadteetmto of estimation the and detection in used methods analysis data present We h nerdpwro ai odatv aatcnce AN naver- on (AGN) nuclei galactic active loud radio of power inferred The sr-hG;atop.E srpyis pn uemsiebakholes black supermassive spin; astrophysics; astro-ph.HE; astro-ph.GA; akfrgon;g-c MLDC gr-qc; back/foreground; o tr itiueaon asv lc hole black massive a around distribute stars How

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 ics te hsclefcsta ih otiuet h bevdrdoloud/quiet radio We AGN. observed the of results. to dichotomy contribute simulated might that our effects all physical a reproduces other provide discuss accurately we analytic that and an power, formula derive of We fitting scaling numerical steeper distributions. this spin reproduces hole accurately that black solution realistic depen- for power 1000 the of then P that axis, variations steeper, such polar thick, much the is become around disk can angle the solid dence if However, narrow a most. subtends at jet tens the few a only of variations power frequency, hole angular black total hole the the disk, P on accretion quadratically thin approximately a depends by surrounded output is power assume hole We black horizon the geometries. hole if the field that, through magnetic find flux of magnetic variety total a the pa- and spin that 0.9999) (dimensionless spins <= of a range 0.1<= wide a rameter for systems such of models numerical noacutteps-etna rcsino h pn nacnitn manner. consistent a in spins the takes of formula sepa- precession my their because post-Newtonian happens the when and account holes radii, into black gravitational two of thousands the of of formula is momentum ration my angular makes and which spins simulations, This the N-body provide and radii. merger-trees gravitational cosmological sep- for of with suitable binaries thousands particularly to 704 or applied Apj hundred when Rezzolla, of direction & spin arations (Barausse mag- final in spin the proposed predicts final recently I accurately the I L40) for that direction. results in formula and reasonable the far give magnitude only so formulas spin nitude, the appeared final all simulations the although the for that all formulas show of various results with the literature compare numerical-relativitythe of I results Here the exploiting expressions simulations. to simple made via recently spin been cosmological the have the attempts model study Several to holes. importance black great supermassive of of evolution is system binary black-hole generic a Abstract: spin theory; post-Newtonian holes; Keywords: Eprint: merger Authors: black-hole a from spin final the direction the of modelling in precession of importance The ∝ Ω H 2 http://arxiv.org/abs/0911.1274 ∝ aase Enrico Barausse, h rdcino h pno h lc oersligfo h egrof merger the from resulting hole black the of spin the of prediction The ( a sr-hC;atop.A rq;kcsrci;msiebnre fblack of binaries massive kicks/recoil; gr-qc; astro-ph.GA; astro-ph.CO; / r H ) 2 o tr itiueaon asv lc hole black massive a around distribute stars How n ecnld hti hsseai h pnaoecnproduce can alone spin the scenario this in that conclude we and , ∝ Ω WNotes GW H 4 reven or ∝ Ω r H 6 = n ospouepower produce does and , r H ( a ) shl osat We constant. held is

99 oe esfrG science GW for News & Notes Notes & News for GW science 100 WNotes GW eertn h ia ais u lasapoc ahohraano hi a out way their on again hole.[shortened] other black radius each the approach tidal from always the after but widely radius, of separate tidal 0.1-0.5 binaries the deep-reaching to penetrating ener- such arriving Interestingly, ejection orbit. highest binaries prograde the for a in produce obtained in survive encounters instead but deep are disruption, these to which do doomed deeply gies, Nor not penetrate are cases. that hole the binaries black of even the 20% that of sphere show We tidal the the energy. into ejection on bina- circular the Focusing of for disruption and for mass. distributions ries of probability the independent provide is we is ejection case, higher it distribution planar have fact, energy objects In the lighter Nonetheless, hole. since cases. black velocities, para- the the disruption, of relevant to binary 50% bound the upon in preferentially exactly explore that, remain ejected show to not does we needed star claims, is lighter previous simulations the to calculation of Contrary three-body set space. full smaller meter the much over a advantage that an binary-to-black is Consequently, and separation initial ratio. its mass masses, hole binary of be terms can in results rescaled framework, in simply this problem In the formulate approximation. to three-body us the parabolic allows restricted between stars the ratio binary mass the magnitude and hole of a black order near Center six passage Galactic The a by mass. disruption point binary massive a more of much problem the revist we Center, Galactic the Abstract: Keywords: Eprint: Authors: Problem 3-body Parabolic Restricted the and Stars Velocity Hyper apigagrtm utNs.W s utNs sato osac o modelled for search to tool a as nested MultiNest multi-modal use We the using MultiNest. (LISA) algorithm, Antenna sampling Space Interferometer Laser the with Abstract: Keywords: Eprint: Anthony Lasenby, Authors: evidence using Bayesian signals burst wave gravitational LISA Classifying http://arxiv.org/abs/0911.0288 http://arxiv.org/abs/0911.1136 ai ee;Kbysi hh;Rsi ln M. Elena Rossi, Shiho; Kobayashi, Re’em; Sari, oiae ydtcin fhpreoiysasta a rgnt from originate may that stars hypervelocity of detections by Motivated ecnie h rbe fcaatrsto fbrtsucsdetected sources burst of characterisation of problem the consider We eo,Fra;Gi,Jnta . rf,Pii;Hbo,McalP; Michael Hobson, Philip; Graff, R.; Jonathan Gair, Farhan; Feroz, sr-hG;atop.E srpyis MI N-body EMRI; astrophysics; astro-ph.HE; astro-ph.GA; aaaayi;g-c LC aaee siain erhalgorithms search estimation; parameter MLDC; gr-qc; analysis; data o tr itiueaon asv lc hole black massive a around distribute stars How

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 utNs a eetcsi tigsgaswt inlt-os ai SR slow as (SNR) that ratio show signal-to-noise and with trials signals independent as string of results cosmic suc- present detect present to also can sources We able burst MultiNest were set. string we data cosmic which release the in the of Challenge, three in all Data characterise LISA MultiNest and Mock of detect the application cessfully of sine- an be- round from choose consider last results to we the used present We to be model, can alternatives. burst ratio two evidence alternative these the associated an tween how evidence show As and Bayesian signals, burst model. the Gaussian string compute cosmic and the cusps, with string cosmic from bursts ulbakhlsi egrrmat.I:si evolution spin recoil II: gravitational and remnants. merger in holes black Dual in given are as- waveforms is gravitational difference emitted mass The fractional one. form. the analytic against and small quasi-circular be be or- to The to sumed taken conﬁgurations. spin is equal- arbitrary motion and and bital single-spin binaries for unequal-mass by (2005)] to work 024039 binaries, the mass 71, in [PRD given Gopakumar as coupling, and spin-orbit Königsdörffer order leading under binaries spinning Abstract: Keywords: Eprint: Authors: cou- spin-orbit pling order leading under binaries spins arbitrary unequal-mass with from waveforms Gravitational Keywords: Eprint: Authors: twihteeiec ai eist aortecretmdloe h alternative. the over model SNR correct the the favour with to coincides begins detectable ratio become evidence sources the which the at which at threshold the that at;kcsrci;msiebnre fbakhls spin holes; black of binaries massive kicks/recoil; parts; ∼ n ieGusa inl ihSRa o as low as SNR with signals sine-Gaussian and 7 http://arxiv.org/abs/0910.5931 http://arxiv.org/abs/0910.5729 ese,Manuel Tessmer, ot,M;Vlnei . eeo . op,M;Rskwk,M;Had,F. Haardt, M.; Ruszkowski, M.; Colpi, A.; Perego, M.; Volonteri, M.; Dotti, h ae eeaie h tutr fgaiainlwvsfo orbiting from waves gravitational of structure the generalizes paper The rq;msiebnre fbakhls pn waveforms spin; holes; black of binaries massive gr-qc; crto ic;atop.O sr-hH;atohsc;E counter- EM astrophysics; astro-ph.HE; astro-ph.CO; discs; accretion o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW ∼ .I ohcss eshow we cases, both In 8.

101 oe esfrG science GW for News & Notes Notes & News for GW science 102 WNotes GW apeo asv lc oebnre a ein<0k/ uhsalrta the spins. than of smaller distribution much isotropic km/s an simulated <70 from median a resulting has from median binaries inferred hole velocities black massive recoil small of of relatively sample a distribution bi- receives Keplerian The coalescence a their recoil. of from gravitational resulting formation hole after black set relic black directions black the massive nary, spin each the disc If the near cooler rotation. preserving flow disc’s a coalesce accretion the in the holes of Alignment coherence of large-scale coherence disc. the reflects higher warmer that the a hole to for due degrees effective direction <30 more the spin and for is the disc, degrees <10 in cold of off-set a level residual the of at A case remains, momentum Myr). angular orbital (<1-2 the of timescale to momentum relative short angular the a orien- with initial on spins their orbit the of align their memory to loose suffice torques spins small-scale accretion hole as the black tation, with the changes that coupling spin find gravito-magnetic We its its disc. grows, to accretion mass due hole direction black and the strength As in is momentum. that angular gas accrete net and or a rotation, co carrying disc’s eccentric the initially to from relative inwards orbits a coplanar spiral of counter-rotating holes relic disc, black circumnuclear The a merger. inside galaxy orbiting gas-rich holes black dual massive of evolution Abstract: ol nraewt nraigsi.I h poielmt ecnr through radius radius inner confirm inner spin. the we tilt, on the zero dependence limit, of expected that limit the opposite be the approximately in the recovers even that, In disks may untilted it of spin. simulations tilts, numerical likely increasing larger is with result for This increase that spin. would such of independent (H/r tilt, nearly disks on is thick radius dependent moderately inner for the that, degrees), find range (15 the we tilt Over 0.9, answers. <= wrong of a/M quite estimates give <= black-hole can different 0 differing procedure of a with such number disks that accretion a show tilted we comparing spins, of By simulations from spin. radius disk the inner accretion the infer surrounding a to of that radius inner using the and measuring actually by is hole black Abstract: holes black permassive Keywords: Eprint: Authors: Accretion Hole Black Tilted Disks of Radius Inner Effective http://arxiv.org/abs/0910.5721 rgl,P Chris P. Fragile, sn ihrslto yrdnmclsmltos eepoetespin the explore we simulations, hydrodynamical resolution high Using n ftepiaymaso eemnn h pno nastrophysical an of spin the determining of means primary the of One crto ic;atop.E srpyis Mcutrat;si;su- spin; counterparts; EM astrophysics; astro-ph.HE; discs; accretion o tr itiueaon asv lc hole black massive a around distribute stars How a 1 2010 21, May

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.)wt modest with 0.2) oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 n h fetv n oyFormalism Body One Effective the Background and Schwarzschild a in Force Self Gravitational lyti oe nterdaintase nerto ocmuetelmnst at luminosity the compute to integration em- transfer We radiation effects. the blackbody in incorporate model to this modified ploy law opacity absorption and Kramer’s system plasma by the Maxwellian from given a transfer from radiation emission study bremsstrahlung we incorporating end, this To hole. black super-massive Abstract: holes black of binaries Keywords: Eprint: Authors: holes black binary per- by disks turbed from emissions electromagnetic Post-merger Abstract: Keywords: Eprint: Authors: rdhf"GFfnto dfie ln h euneo iclrorbits). circular of sequence gauge-invariant the certain, along a (defined entering function logarithm GSF level, first "redshift" expan- (4PN) the post-Newtonian post-Newtonian compute fourth analytically the the at we entering functions and GSF) start and terms (EOB zoom-whirl various logarithmic zero-binding of sions that special a show on We focussing by orbit. or orbits, either We eccentric computations: GSF formalism. studying from EOB by information the more obtaining constrain of to ways data various which NR suggest parameters) comparable-mass EOB coming using some information after (among The degeneracy left the was holes. break to black helps binary numeri- data the coalescing GSF high-accuracy with from on to information data formalism this (NR) EOB fre- combine relativity the orbital we cal comparing the and by orbit, obtained of circular recently shift stable one the first-GSF-order last from the the extracted One-Body of of be Effective quency calculation can the which GSF of information published blocks the recently building back- display Schwarzschild basic We a the in Hamiltonian. about moving (EOB) us mass point inform a can on ground effects (GSF) Force Self itational http://arxiv.org/abs/0910.4969 http://arxiv.org/abs/0910.5533 nesn ate;Lhe,Li;Mgvn,Mge;Nisn David Neilsen, Miguel; Megevand, Luis; Lehner, Matthew; Anderson, Thibault Damour, edsusvroswy nwihtecmuaino osraieGrav- conservative of computation the which in ways various discuss We esmlt h osbeeiso rmads etre yarecoiling a by perturbed disk a from emission possible the simulate We fetv n oy MI rq;ps-etna theory post-Newtonian gr-qc; EMRI; body; one Effective crto ic;atop.E srpyis Mcutrat;massive counterparts; EM astrophysics; astro-ph.HE; discs; accretion o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW

103 oe esfrG science GW for News & Notes Notes & News for GW science 104 WNotes GW osriigteiiilms ucino tr nthe in stars of function Centre mass Galactic initial the Constraining signals electromagnetic for esti- work the emission above and previous thermal results from transfer simple luminosity radiation bremsstrahlung a the com- mated between with the agreement and close over frequencies) find integrated We all is model. emissivity over the and which domain (in putational limit transparent a estima- from luminosity bremsstrahlung tions previous with compare and frequencies, several Eprint: Authors: Binaries Hole Black of Coalescing Phase Ringdown the from Recoil Gravitational-Wave high as such do properties and region’s mass. etc. the IMF luminous field of canonical tidal result missing strong the a metallicity, the density, as with variation for consistent systematic up is a expected make suggest Centre SBHs not Galactic to of the enough number that just the conclude is since We IMF core, both canonical observed and a the cluster time central from of first the extent the of For and mass Centre. presence dynamical Galactic and the the luminosity in the observed explain as the we core turning here a friction, into dynamical stars Further- to visible due observations. of centre the cusp the with towards consistent and migrate (SBHs) ratio SBHs holes mass-to-light these black more, a over stellar in formation of results mass star IMF total continuous canonical a by a contrast, inferred following In explained mass lifetime be region. Galaxy’s of to the this amount high in show limited too kinematics we the stellar is codes considering from parsec IMF, different central top-heavy using the long-standing models in variation a evolution luminosity significant stellar a observed for of the reason means that the By be IMF. may Way the Milky the of of centre the in stances Abstract: holes black supermassive dynamics; Keywords: Eprint: Authors: disk. the of period orbital the to connected variability intensity strong a in resulting 10 http://arxiv.org/abs/0910.4594 http://arxiv.org/abs/0910.4960 14 ic lxnr e lnht u;Wl,Cifr M. Clifford Will, Luc; Blanchet, Le; Alexandre Tiec, Pavel Kroupa, Holger; Baumgardt, Ulf; Loeckmann, arde)Hr edsusteqeto hte h xrm circum- extreme the whether question the discuss we Here (abridged) z o oe rqece,w n efelpigbhvo ntedisk, the in behavior self-eclipsing a find we frequencies, lower For Hz. sr-hC;atop.A srpyis -oy aitru * stellar A*; Sagittarius N-body; astrophysics; astro-ph.GA; astro-ph.CO; o tr itiueaon asv lc hole black massive a around distribute stars How

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 5pretoe ierneo asrto,wt aiu eoiyo 8 km/s 180 of velocity maximum a 0.38. with of ratios, ratio 10- mass mass to a of relativity at range numerical wide from a those with over agree percent velocity 15 kick phases, net ringdown significant the and for second a merger results inspiral, produces to our to due radiation accurate contributions ringdown the data Adding that initial "anti-kick". prove using We solution equations a order. Zerilli on post-Newtonian based and and Regge-Wheeler phase, ringdown the the of during calcu- emitted approximation" to radiation "close-limit the up a of (ii) accumulated lation holes, velocity black non-spinning kick two earlier of the an merger of the (i) theory, combine We post-Newtonian using gravitational phenomenon. of calculation, important emission anisotropic astrophysically the an by is caused radiation, and holes, black orbiting two of Abstract: theory Newtonian Keywords: oe,adcrua ris o hc ohee n d oe otiue na holes. black In pro- binary recoil coalescing gravitational contribute. of the phase modes of ringdown study odd the the and during to duced applied even is both formalism which this work, for separate even orbits, in of obtained circular only composed is and momentum, waveform modes, zero-angular ringdown with equa- collision The wave head-on numerically. Zerilli cases: evolve two and then Regge-Wheeler we the which for tions, conditions co- these initial use build We to equations. efficients perturbation field linear perturbative the the 2PN-accurate the of describing satisfy components coefficients consistently (axial) multipolar odd-parity and The of polar) that (or with hole. even-parity identified black and Schwarzschild form of perturbed CL metric approximation in a 2PN expanded (CL) The formally close-limit is the conditions. binaries point-particle of initial (2PN) means second-post-Newtonian by from described starting is holes black orbiting Abstract: forms Keywords: Eprint: Authors: Conditions Initial Binaries Post-Newtonian Hole with Black for Approximation Close-limit The http://arxiv.org/abs/0910.4593 ic lxnr e lnht Luc Blanchet, Le; Alexandre Tiec, h rvttoa eolo kc"o lc oefre rmtemerger the from formed hole black a of "kick" or recoil gravitational The h igonpaeo lc oefre rmtemre ftwo of merger the from formed hole black a of phase ringdown The rq;msiebnre fbakhls otNwointer;wave- theory; post-Newtonian holes; black of binaries massive gr-qc; rq;gaiainlrci;msiebnre fbakhls post- holes; black of binaries massive recoil; gravitational gr-qc; o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW

105 oe esfrG science GW for News & Notes Notes & News for GW science 106 WNotes GW osdrda osbecoigmcaim.Hneteflwgvrsmc lower much governs flow the Hence temperature electron mechanisms. cooling are black photons possible a soft as towards of considered Comptonization infall inverse its and during synchrotron phases Bremsstrahlung, various advec- hole. state, through general steady passes that in flow show model accretion we disc tive self-consistently, accretion processes sub-Keplerian cooling global explicit a including around on versa Based vice and holes. phase dominated black cooling a to flow accreting temperature two Abstract: Keywords: Eprint: Authors: around discs accretion holes temperature black two in domi- phase cooling nated to inefficient radiatively from Transition aitru * uemsiebakholes black supermassive A*; Sagittarius Keywords: Eprint: Authors: high to low explain sources to luminous processes cooling various pres- of in ence paradigm flow advective general holes: of black Description rotating around accretion temperature Two heats. specific of ratio PKS rate, accretion (e.g. mass quasars (e.g. of ultra-luminous combinations and sources different AGNs X-ray at luminous ultra-luminous 0743-67) highly A*), the as Sgr of well luminosities as (e.g. observed SS433), quasars the and reproduce AGNs to under-fed able be radiatively successfully the to is is expected which flow differ- is counterpart The flow viscous two inefficient. highly viscous for its weakly solutions to a compared the that dominated conclude compare cooling and finally viscosity We of regimes binaries. ent X-ray emitted gamma-rays and and X-rays AGNs hard from the explain potentially may solutions the fore, ∼ 10 10 . 2 http://arxiv.org/abs/0910.4502 http://arxiv.org/abs/0910.4818 − ih,Mnk;Rjs,S . uhpdyy Banibrata Mukhopadhyay, R.; S. Rajesh, Monika; Sinha, aeh .R;Mkoaha,Banibrata Mukhopadhyay, R.; S. Rajesh, 10 eivsiaetetasto fardaieyiefiin hs fviscous of phase inefficient radiatively a of transition the investigate We crto ic;atop.E srpyis uemsiebakholes black supermassive astrophysics; astro-ph.HE; discs; accretion 11 crto ic;atop.E srpyis Mcutrat;gr-qc; counterparts; EM astrophysics; astro-ph.HE; discs; accretion . 8 nterneo crto aei digo nt .1-10 There- 100. - 0.01 units Eddington in rate accretion of range the in K o tr itiueaon asv lc hole black massive a around distribute stars How ∼ 10 8 − 10 9 . 5 oprdt h o rtn ftemperature of protons hot the to compared K

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 Abstract: eiain hssmlfiddrvto a eueu o eaoia purposes. Finn’s pedagogical for of useful version be simplified may derivation a simplified recovers This interferometers, derivation. describe and pitfalls, to these adapted avoids timing when pulsar wave and gravitational several tracking the doppler of contains spacecraft derivation for contemporaneous detector response a wave that out gravitational point I interferometric Here an errors. of response the of Abstract: Keywords: Eprint: Authors: detectors wave interferometric gravitational of response the of derivation Alternative oiiso h ne-e Gsadqaas(..Sgr (e.g. lumi- quasars observed and the reproduce AGNs finally radiatively under-fed we is the hand, which of in counterpart nosities solutions viscous the highly all its inner With the to inefficient. at compared particularly disc, dominated, the cooling be of to region expected is flow viscous weakly a and X-rays hard h uioiyosre ntehgl uiosAN n lr-uiosquasars appropriately ultra-luminous predicts and 0743-67). also AGNs PKS luminous solutions (e.g. highly of the set in The observed ac- luminosity heats. mass the as specific such of parameters ratio input rate, of cretion combinations different at SS433), (e.g. sources temperature temperature electron Hence lower versa. much vice and governs advection phase of flow inefficient phases the radiatively various to through paradigm passes advective transition horizon, general sub-Keplerian event – to hole is Keplerian black It the the from 0.998. to infall parameter region its Kerr during a flow, with the holes that black accretionfound Kerr mass and super-Eddington Schwarzschild around and rates cooling Eddington possible as sub-Eddington, considered for are photons mechanisms, soft of Comptonization sub- inverse a and synchrotron with Bremsstrahlung, selfconsistently. flows processes cooling accretion equa- explicit of conservation including underlying tions solution the solving global by profile, the momentum describe angular Keplerian We holes. black tating crto aei digo nt .1< 0.01 units Eddington in rate accretion http://arxiv.org/abs/0910.4372 ons,Ni J. Neil Cornish, thsrcnl enpitdotb inta h ogsadn derivation long-standing the that Finn by out pointed been recently has It eivsiaetevsostotmeaueaceindssaon ro- around discs accretion temperature two viscous the investigate We rq;isrmns interferometers instruments; gr-qc; ∼ 10 o tr itiueaon asv lc hole black massive a around distribute stars How γ 10 ry mte rmAN n -a iais ete hwthat show then We binaries. X-ray and AGNs from emitted -rays . 2 − 10 11 . 8 .Teeoe h ouinmyptnilyepanthe explain potentially may solution the Therefore, K. ∼ WNotes GW M ˙ < ∼ 0,cmae otehtpoosof protons hot the to compared 100, ∼ 10 A 8 ∗ outalmnu X-ray ultra-luminous to ) − 10 9 . 5 ,i h ag of range the in K,

107 oe esfrG science GW for News & Notes Notes & News for GW science 108 WNotes GW Abstract: observations holes; Keywords: Eprint: A. F. Primini, Authors: Chandra with G1 Cluster Globular the Hole in Black Intermediate-Mass the of Localization X-Ray n o-iglrcodnt ace.Hr ecnie eua atsa near Cartesian regular a consider we Here communicat- multiple patches. with coordinate covered be non-singular to ing spacetime generalised the in allowing differences and finite coordinates, implementing approach, moving-puncture the ing Abstract: relativity Keywords: Eprint: Peter Authors: ex- zone an wave with tended simulations hole black binary accuracy High G1. of center the at hole Future black companion. emission. intermediate-mass a radio an whether is the from reveal there from will accretion offset observations imaging be to radio may high-sensitivity due emission and are high-resolution X-ray the X-rays seems that the gas find that also cluster We Eddington suggest the the we to from X-ray accreting and hole, of hole unlikely black ratio emis- intermediate-mass black the X-ray central intermediate-mass on the a Based an of of luminosity, binaries. origin accretion X-ray core either the low-mass to the for ordinary due within or possibilities be from two could comes are it G1 There sion: of cluster. emission the X-ray of the radius that XMM- conclude by measurement We 1sigma previous the a than Newton. derive smaller we significantly images, 0.15", with CFHT of Telescope and radius detected error HST Space clearly with Hubble cross-registering is Observatory, by G1 and X-ray (CFHT). Chandra Chandra Telescope the Canada-France-Hawaii using and by (HST), M31 in G1 ter http://arxiv.org/abs/0910.3803 http://arxiv.org/abs/0910.3944 ole,Dns eswg hita;Shetr rk obn,Nl;Diener, Nils; Dorband, Erik; Schnetter, Christian; Reisswig, Denis; Pollney, og .K . ene .O;D tfn,R;Brb,P;Lwn .H G.; H. W. Lewin, P.; Barmby, R.; Stefano, Di O.; C. Heinke, H.; K. A. Kong, epeetrslsfo e oefrbnr lc oeeouin us- evolutions hole black binary for code new a from results present We erpr h otacrt -a oiino h in lblrclus- globular giant the of position X-ray accurate most the report We rq;msiebnre fbakhls ueia ehd;numerical methods; numerical holes; black of binaries massive gr-qc; sr-hH;atohsc;goua lses nemdaems black intermediate-mass clusters; globular astrophysics; astro-ph.HE; o tr itiueaon asv lc hole black massive a around distribute stars How

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 nldn h eovdhge amnc,aecnegn n a econsistently be can and convergent are waveforms, to The harmonics, extrapolated merger. higher dur- during resolved 0.090% 0.153% the and and 0.010% including 0.003% the than and determine better respectively, we accuracies inspiral, merger), numerical ing before to non- orbits amplitude equal-mass 8 an and than of phase more inspiral for the (evolved of binary test-case the spinning from well-studied disconnected the causally resolu- is For grid which sufficient location measurement. maintain boundary to outer us artificial an allow result- to coordinates efficiencies tion adapted The of zone. use wave the the from covering ing grids spherical adapted with zone, h esrmn ftebakhl pnbsdo h pcrlfitn n influence and fitting spectral the on luminosity. based of dependence influence spin angular will hole the effects black these the Consequently, of measurement spectra. signif- the have emergent advection the heat the accretion on and the influence thickness inclination disk icant of large the region both rate, spin, accretion inner hole high black the At large spectra. and in emergent the escape the in to will trapped contribute disks and radiation disk accretion effect, the advection of heat region moderate the outer at of that inclusion find We with effect. rate, self-shadowing accretion disk disk discussed. the self-consistent are consider use rate we we that and accretion disk are equations and works of spin previous effect hole to the compared black and improvements the The advection depen- of heat estimation angular the the of The on effects thickness the luminosity, method. disk emergent ray-tracing the resulting of relativistic The dence using work. calculated this in are investigated spectra are disks accretion slim ativistic Abstract: holes black supermassive spin; parts; Keywords: Eprint: Authors: Self-Shadowing Disk and Black Trapping Photon Kerr of Effect Surrounding Holes: Disks From Spectra Emergent lst erbakhl ihirdcbemass irreducible set- with remnant hole the black that Kerr confirmation a strong to a tles providing 0.01%, within to (to calculations modes these for frequencies Ringdown down. S f / M 2 f = http://arxiv.org/abs/0910.3530 0 i un-ig un eFi a,Xinwu Cao, Ye-Fei; Yuan, Guang-Xing; Li, ae nanwetmto ftertikes h lblpoete frel- of properties global the thickness, their of estimation new a on Based . 686923 crto ic;atop.A sr-hH;atohsc;E counter- EM astrophysics; astro-ph.HE; astro-ph.GA; discs; accretion r o tr itiueaon asv lc hole black massive a around distribute stars How ∞ → ± 10 × hogottesmlto,icuigtemre n ring- and merger the including simulation, the throughout 10 − 6 WNotes GW M irr ( `, = m 0 ) . 884355 = (6 , 6) ac perturbative match ) ± 20 × 10 − 6 n spin and

109 oe esfrG science GW for News & Notes Notes & News for GW science 110 WNotes GW efeunl eueae vrteps 0 y,wihad e hleg to gas challenge of new problem holes. longstanding a black the adds massive to into insights or which fueling provides persist Myr, and should 200 formation orientation) disk past stellar that similar the the the imply a of over also with but part rejuvenated structure HVSs warped frequently disk of outer be the origin the (or GC by the disk support deﬁned central only plane arm the not northern the results the or Our of plane GC disk. the the CWS with in correlated orientation be mini-spiral an may the HVSs with from of of structure originate rest stellar HVSs The disk-like the it. existed of to previously similar most with a that consistent or suggests is disk which plane CWS be- disk, one the with of CWS orientation consistent (inner) The the spatially of planes. are disk that HVSs thin discovered two the on directly. located all progenitors ing almost their of that population ﬁnd HVSs parent of also the We distribution of spatial distribution the spatial Therefore, the progenitor. maps to its anti-parallel of almost is direction HVS injecting an the of direction and ejecting arguments the analytical i.e., clockwise- both simulations, using numerical a progenitors memo- their for- well in of their can directions and HVSs hosted injecting that the MBH demonstrate being rize the we paper, from many this parsec In with a puzzles. half remaining GC, mation within the disk (CWS) in stellar populated young rotating also unknown. progenitors are their stars with stars OB the B-type in mainly (MBH) are hole(s) They black (GC). massive Center the Galactic with stars of interactions of products namical Abstract: dynamics Keywords: Eprint: Authors: hyperveloc- stars of origin ity the and distribution spatial the On c;sprasv lc holes black supermassive ics; Keywords: Eprint: Authors: gravitational- black lower-frequency massive astrophysics for wave a Implications around segregation hole: mass strong On http://arxiv.org/abs/0910.3206 http://arxiv.org/abs/0910.3260 u ojn hn,Fpn;Y,Qingjuan Yu, Fupeng; Zhang, Youjun; Lu, rt,Mge;AaoSon,Pau Amaro-Seoane, Miguel; Preto, yevlct tr HS)ecpn wyfo h aatchl r dy- are halo Galactic the from away escaping (HVSs) stars Hypervelocity sr-hC;atop.A srpyis MI -oy tla dynam- stellar N-body; EMRI; astrophysics; astro-ph.GA; astro-ph.CO; sr-hG;atohsc;ER;osrain;SgtaisA;stellar A*; Sagittarius observations; EMRI; astrophysics; astro-ph.GA; o tr itiueaon asv lc hole black massive a around distribute stars How

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 aeour pare segregation Abstract: Abstract: holes black supermassive ics; Keywords: and VLT from SgrA* Authors: around S2 star data Keck the of orbit The The space. energy in equation (FP) Planck hsms ag.SneER ae cl as scale in rates MBHs EMRI around Since common range. be mass may this cusps stellar segregated, mass quasi-steady, that associated scales time the than that longer show not are we Way, stars re-growth Milky giant cusp the of with dearth of a region revealing sub-parsec observations of the recent fraction in of small view (realistically) In a is population. stars total heavy the of fraction the number confirm the both when but regation solution, FP the in than hre hnaHbl iefrbakhlsmasses holes black for time Hubble a than shorter .9ss p n (B)=43 -02(tt -0.30(sys) +- fit. +- 0.15(stat) multi-star 0.20(stat) +- a +- 8.28 from 4.30 = = R0 M(MBH) obtain and We kpc and frame. errors 0.29(sys) reference A*, systematic the Sgr for by of to dominated allows calibration are distance long-term set numbers and the data these of of combined mass accuracies so of overall errors The the statistical but (2008). the with of consistent al. improvement are moderate et frames a Ghez reference the in the in given offsets of required be uncertainties origin The the can the sets. sets of in data two offset velocities two the small and the of a coordinates frame that for reference allowing show the when of we other definition letter each the this with agreement In excellent to when the sets. brought match of two not and center do the positions independent the overplotting measured are in simply the sets hole though data even black astrometric results, two massive consistent The the yielded orbits. to stellar distance using the Way and Milky of mass the mated Eprint: R. Genzel, T.; Ott, O.; cusps. stellar segregated strongly from originate should events these http://arxiv.org/abs/0910.3069 N ilse,S;Esnae,F;Fiz .K;Brk,H;DdsEe,K;Pfuhl, K.; Dodds-Eden, H.; Bartko, K.; T. Fritz, F.; Eisenhauer, S.; Gillessen, epeet o h rttm,aclear a time, first the for present, We w eetppr Ge ta.20,Glesne l 09 aeesti- have 2009) al. et Gillessen 2008, al. et (Ghez papers recent Two ouinfrteselrdsrbto rudamsiebakhl.W com- We hole. black massive a around distribution stellar the for solution bd eut ihtoeotie ysligteobtaeae Fokker- orbit-averaged the solving by obtained those with results -body sr-hG;atohsc;osrain;SgtaisA;selrdynam- stellar A*; Sagittarius observations; astrophysics; astro-ph.GA; o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW (0 . M 1 N • − − robustness bd ergto ssihl stronger slightly is segregation -body α N 0 with , . bd elzto fthe of realization -body 25) M × • α . T ∈ rlx ftergm fsrn seg- strong of regime the of 4 [1 × ( × r h / 10 10 ) 4 hs iesae are scales time These . , 6 6 1] M M odfato of fraction good a ,

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111 oe esfrG science GW for News & Notes Notes & News for GW science 112 WNotes GW nua itiuino h pn ihrsett h nlobtlaglrmomen- angular orbital final the to perform the We respect compute L. with we spins tum, separation, fiducial the final of perform this distribution we At ri=50m, angular rf=5m. of dif- to separation for initial down S1=S2=0.97 fiducial evolutions magnitudes a 3.5PN from and Starting uni- S2 random ratios. and remnant a mass S1 with the ferent directions start of spin we distributions regime, of inspiral the distribution the as form For velocity. well recoil as and merger, spin, and mass, inspiral the during naries Abstract: Keywords: Eprint: Manuela Authors: Binaries Black-Hole Spinning of studies Statistical hoyo eea eaiiyweeteieainsat rmteNwo hoyof theory Newton the from starts iteration the where relativity general of theory Abstract: Keywords: Eprint: Authors: binary problem the on results Analytic methods: Post-Newtonian distrib- universal a show magnitude at spin peaked along black-hole highly distribution final ution angular The as peaked axis. highly decays orbital a final and distribution the 1000km/s, velocity than larger recoil recoils the of ity of mass magnitude binary’s the the as that P well found as cho- We magnitudes randomly and for spins formulae ratio. ar- individual those with the evaluate binaries of then We directions black-hole nu- sen merging spins. full for and velocity to ratios recoil mass turn remnant and bitrary final we spin, the binaries, describe mass, to black-hole hole formulae black of empirical merger introduce We both the techniques. of study merical counter-alignment To di- but towards S, small distribution products. and a the L find scalar We of and momentum. Delta bias angular and significant total L statistically and velocities between recoil angles to the related of rectly distribution the compute and otefia ria nua momentum. angular orbital final the to ( v exp ) http://arxiv.org/abs/0910.2857 http://arxiv.org/abs/0910.3197 − cafr Gerhard Schaefer, v esuytesaitcldsrbtoso h pn fgnrcbakhl bi- black-hole generic of spins the of distributions statistical the study We ealdacuti ie napoiainshmst h Einstein the to schemes approximation on given is account detailed A oso alsO;Nkn,Hryk;Zohwr oe;Campanelli, Yosef; Zlochower, Hiroyuki; Nakano, O.; Carlos Lousto, / eea eaiiy rq;msiebnre fbakhls spin holes; black of binaries massive gr-qc; relativity; general rq;msiebnre fbakhls otNwointer;spin theory; post-Newtonian holes; black of binaries massive gr-qc; 2500 km o tr itiueaon asv lc hole black massive a around distribute stars How / s 16 60ms n qt- sqrt and =630km/s, , 4 f S iuain o i asrto ewe = n q=1/16 and q=1 between ratios mass six for simulations / f m 2 = 0 . 73 n 5dgesmslgmn ihrespect with misalignment degrees 25 a and =54ms edn oa2%probabil- 23% a to leading 534km/s, 2= ˆ

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 lctfrst ihrps-etna res h eiaeueo lc oe in general holes in black function of delta use Dirac discussions. the delicate find of relativity The and ex- calculations orders. in expansion presented post-Newtonian post-Newtonian are higher point binaries to pure spinning forms of ro- fluids, plicit Hamiltonians modelling Various ideal moments mass-quadrupole are holes. and black models spin tating matter with masses treated point The and masses, post-Newtonian emphasized. and to expansions near is multipole the of schemes fitting in natural performed The are zones. (radiation) expansions Poincaré far Post-Newtonian the and introduced. identified are is systems Donder algebra isolated Fock-de Arnowitt, Lorentz-covariant of the quantities of of Conserved formalism ones approach. harmonic canonical the the and of Misner and ones Deser, field isotropic Einstein the generalized represent the to used equations, are conditions coordinate different Two gravity. Abstract: Keywords: Eprint: Authors: galaxy in relations scaling mergers Hole Black of evolution The h itr nwihsprasv H eeo infiatybfr hi parent their before significantly develop disfavor BHs the thus supermassive onto simulations bulges. which evolve our in implication BHs picture By overmassive the which mergers. in fact gas-rich that scenario The through indicates the relations, relations the out remnants. onto rule merger evolve not over simulations the do dominating our of relations the relations, stage above observed evolutionary starting BHs the the that in from scatter arising of scatter source log the prime (Delta ( the fractions cases is gas all fraction initial in high relations have the log progenitors above (Delta the them which above remaining in still Mergers but relations, the towards evolve log log (Delta (Delta there stay relations ( relations the the fractions onto gas evolve initial relations low the with the below of Progenitors coalescense BHs. final the their after and established galaxies rapidly are relations final The relations. h iuain ihtepoeio lc oemse en ntal eo (Delta below initially being masses hole black log progenitor the with simulations the M bulge M BH lnsa ucino iei ikglxe negigmres ebegin We mergers. undergoing galaxies disk in time of function a as planes http://arxiv.org/abs/0910.2232 -) n(et log (Delta on =-2), oaso,PtrH;Bret nra;Na,Thorsten Naab, Andreas; Burkert, H.; Peter Johansson, esuyteeouino lc oe Bs nthe on (BHs) holes black of evolution the study We sr-hC;atohsc;csooy uemsiebakholes black supermassive cosmology; astrophysics; astro-ph.CO; o tr itiueaon asv lc hole black massive a around distribute stars How M BH 0 n bv Dlalog (Delta above and =0) M BH 0 n nlypoeiosaoeterelations the above progenitors finally and =0) WNotes GW M BH 05.W n htteiiilgas initial the that find We =0.5). M M BH BH 05 h bevdlocal observed the =0.5) -.8,poeioson progenitors =-0.18), M BH f gas f − gas 02 starting =0.2) σ 08 evolve =0.8) and M BH =0.35). M BH −

113 oe esfrG science GW for News & Notes Notes & News for GW science 114 WNotes GW s25% eedn nteaotdSB vlto oe.O h te hand, other (masses the binaries On massive level by model. produced precision evolution bursts nanosecond detecting SMBH one of adopted a probability the find the at on burst we depending resolvable criterion, 2-50%, a resolvability catching is basic of re- a chance assess Implementing the to required that sources. be would such same study of the analysis in solvability data emitting detailed binaries confu- A SMBH underlying ’standard’ the window. other in frequency the out all washed by be produced will noise sion bursts such of most However, (PTAs). with residuals ≥ Keywords: Eprint: Rainer Spurzem, Junichiro; Makino, Christoph; Eichhorn, Matthew; Astrophysics, Authors: holes: Detection and black Waves Gravitational supermassive of Triplets Keywords: Eprint: Authors: Galaxies Triaxial in Masses Hole Black Estimating masses with SMBHs of models timing ( pulsar ulation Antenna with Space bursts Interferometer these Laser than of the higher detection and of substantially likelihood frequencies The at frequency. periapsis. orbital signal orbital the wave at gravitational emitted be a as can produces high radiation This (as gravitational of eccentricity bursts galaxy high intense within triple very phases, triples hole of of black dynamics phases not a the exhibit of do of cores formation simulations binaries the Numerical these galaxy, possible. If third is a system galaxies. with host merger their the of before coalesce merger to struc- expected the cosmological are following SMBHs the binaries scenarios, in form formation role hierarchical active In fundamental process. a formation ture play to recognized been have Abstract: holes black supermassive dynamics; stellar N-body; 0 . 1 LISA ntil ytm efidta e ofwdzn fteebrt ilproduce will bursts these of dozens few to few that find we system, triple in http://arxiv.org/abs/0910.0844 http://arxiv.org/abs/0910.1587 oc,RmoC .vndn eZew .Tim P. Zeeuw, de den; van E. C. Remco Bosch, > uemsiebakhls(MH)fudi h etr fmn galaxies many of centers the in found (SMBHs) holes black Supermassive snegligible. is mr-eae a;Ssn,Abro ofa,Lrn Benacquista, Loren; Hoffman, Alberto; Sesana, Pau; Amaro-Seoane, sr-hC;atop.A srpyis uss omlg;GAEhw; GRAPE cosmology; bursts; astrophysics; astro-ph.GA; astro-ph.CO; sr-hC;atop.A srpyis uemsiebakholes black supermassive astrophysics; astro-ph.GA; astro-ph.CO; 1 s ihntesniiiyrneo otcmn usrtmn arrays timing pulsar forthcoming of range sensitivity the within ns, o tr itiueaon asv lc hole black massive a around distribute stars How & 10 7 LISA M a 1 2010 21, May suigafato fbinaries of fraction a Assuming . setmtduigsvrlpop- several using estimated is ) e ∼ 0 . 99 .Drn these During ). & 10 7 M

) oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 rnucdipc nbakhl eorpy ic ogl hr ftemost the of third a triaxial. roughly strongly since are demography, galaxies hole massive black have axisymmetric may on effect the impact this of However, pronounced that relationship. a of M-sigma errors the the with within consistent and still par- model is This estimate model. mass axisymmetric hole the best-fitting to black our respect that ticular find with we doubles and estimate to triaxial mass our mildly identical hole is in black shape is included best is estimate the twist 3379, mass kinematical NGC degrees of hole model 5 black observed axisymmet- the our an When and using studies. edge-on accurately previous modeled nearly be viewed only of shape can effect and M32 ric M32 the that galaxies find explore We studied to previously 3379. models the NGC orbit-based on triaxial assumption axisymmetric general the fully relaxing use spher- we or spheroids Here oblate axisymmetric ical. are galaxies that assumption the use matics Abstract: e bevdadrs rm oosadpoete.W on htXryselected X-ray that found We properties. galax- host and the colors studied frame ( 2) rest observation; sources and Chandra 179 the observed of rates. in ies detected association formation area X-ray/infrared/optical star MUSIC the and the refined in masses 1) stellar photometric we: as of particular, determination such In reliable parameters, as galaxy the well observations and as of K-band redshifts sources identifications deep X-ray accurate the galaxies. which ensuring of host for available, counterparts their area, are and MUSIC ISAAC@VLT Galac- the observation with Active to 1Ms obtained observational obscured analysis CDFS of modern the the properties in limited in the We topics detected of important (AGN) study most Nuclei a the tic present of we one Here is cosmology. centre their in side Keywords: Eprint: V. Mainieri, A.; Fontana, F.; Civano, A.; Merloni, G.; Hasinger, Authors: in South z=0.6-4 Field at Deep Activity Chandra the Starburst and Growth Hole Black rmifae igotc.Tehs aaiso -a eetdosue G are AGN obscured selected AGN X-ray as of selected galaxies ( been massive host all have The not diagnostics. would infrared latter from the continuum; infrared dominated es o G fsmlrluminosities. similar of AGN for verse Abstract: holes black 1SF1and (1/SSFR1 L X > 10 http://arxiv.org/abs/0910.1007 42 oto h ue asv lc oems siae ae nselrkine- stellar on based estimates mass hole black massive super the of Most rs,M;Foe . atn,P;Gain . oati . aoai G.; Zamorani, A.; Comastri, A.; Grazian, P.; Santini, F.; Fiore, M.; Brusa, ergs h oeouino otglxe n h ciebakhlswihre- which holes black active the and galaxies host of co-evolution The M sr-hC;atohsc;csooy bevtos supermassive observations; cosmology; astrophysics; astro-ph.CO; − M ∗ 1 G hwSizrclr ossetwt ohANadstarburst and AGN both with consistent colors Spitzer show AGN ) > ∗ o tr itiueaon asv lc hole black massive a around distribute stars How > 10 3 10 x M 10

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115 oe esfrG science GW for News & Notes Notes & News for GW science 116 WNotes GW hs ocpsi civn itrac euto o pc-ae eetr beyond detectors space-based LISA. for by of reduction each dominated disturbance of achieving disadvantages spectrum, in concepts and frequency those advantages discuss the ultimately of and noise, region acceleration ’low-frequency’ sen- the strain expected in compare concepts, sitivities payload LISA different for four requirements reduction describe fu- disturbance beyond, for discuss and design we realistic paper, a this with In pushed mission. be ture can noise ultimately acceleration and low reduction, how disturbance understand improved to achieving is of motivation possibility general investi- the The currently Germany. exploit Astrium, are EADS and and Stanford, LISA HEPL, beyond at gated applications have potential and concepts promising with (LISA) several proposed Antenna Nevertheless, maturity. been Space of Interferometer level Laser high the a reached for has sen- baseline cubical current two the with is conﬁguration sens- sors A demanding requirements. extremely reduction with disturbance and Sensor ing Reference Gravitational a require physics Abstract: Keywords: Eprint: U. Johann, L.; R. Byer, W.; Fichter, P.; Gath, Authors: performance noise in- acceleration space-based terferometers: future for concepts drag-free Advanced lc oe neatsrnl ihec te n lc oebakhl iaisare binaries hole hole-black black the and core other the each In with strongly expe- concentrated. interact holes centrally holes black become black the and that segregation ﬁnd We mass strong evolution. rience stellar Carlo Monte full self-consistent and a dynamics using of holes, treatment black and stars neutron containing naries Abstract: ics Keywords: Eprint: Authors: Binaries Clusters Hole Globular Black Inside - I Clusters Star in Binaries Compact http://arxiv.org/abs/0910.0546 http://arxiv.org/abs/0910.0758 onn,J .B;Bncusa .J;Ges,M;Suzm R. Spurzem, M.; Giersz, J.; M. Benacquista, B.; M. J. Downing, ead,D;Aln . oki,J . u,KX;DBa . uha,S.; Buchman, D.; DeBra, K-X.; Sun, W.; J. Conklin, G.; Allen, D.; Gerardi, esuytecmatbnr ouaini trcutr,fcsn nbi- on focusing clusters, star in population binary compact the study We uueda-remsin o pc-ae xeiet ngravitational in experiments space-based for missions drag-free Future sr-hH;atop.R srpyis lblrcutr;selrdynam- stellar clusters; globular astrophysics; astro-ph.SR; astro-ph.HE; rq;isrmns interferometers instruments; gr-qc; o tr itiueaon asv lc hole black massive a around distribute stars How

a 1 2010 21, May oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 agt o pc-ae eetr.W ocueta trcutr utb ae into taken statistics. be population must binary interesting clusters compact are predicting star bi- clusters when that hole account conclude star We hole-black that detectors. black suggesting space-based eccentric sources, field for highly targets LISA galactic two potential the find are in also that We merge naries will time. that Hubble escapers a our hard within within mergers many hole the produce hole-black eject but black or no simulations find destroy We also binaries. however, hole interactions, hole-black black strong The efficiently. very formed Eprint: Art the of Authors: State The holes: black of Mass of terms in SED, the processes. as emission Compton well external as and physical self-Compton curves the synchrotron light discuss synchrotron, We contemporaneous (SED). limits the distribution upper energy of derive spectral implications flare to (INTEGRAL/ISGRI) the us gamma-rays of enabled ends soft both which first a at coverage, the from (VLT/VISIR) For infrared benefitted h. mid also X-rays 1-2 and event in for an simultaneously 4th of April observed such detection on horizon, time, (VLT/NACO) the multiwave- the infrared report extensive of near we an vicinity and Herein, of the (XMM/EPIC) target from 2007. main flare April bright the in a out been carried has we It campaign Way. length Milky the of center Abstract: holes black Keywords: the from Authors: flare hole bright black supermassive a Center Galactic on constraints gamma-ray Soft egtn lc oe.Bakhlscnb on nselrbnr ytm nour in systems binary stellar in found be can holes Black holes. black weighting Abstract: holes black supermassive Keywords: . atn . aae .O;Frad,P;Blne,G;Prut . rso N.; Grosso, D.; Porquet, Eprint: G.; Belanger, P.; Ferrando, O.; F. P. Melia, F.; Yusef-Zadeh, Lagage, E.; Pantin, R.; http://arxiv.org/abs/0910.0399 http://arxiv.org/abs/0910.0313 rp . odum . ere,R;DdsEe,K;Glesn . Genzel, S.; Gillessen, K.; Dodds-Eden, R.; Terrier, A.; Goldwurm, G.; Trap, zry . ioau,M. Nikolajuk, B.; Czerny, nti ml eiww rsn h culsaetekoldeabout knowledge the state actual the present we review small this In aitru *(g * stesprasv lc oersdn tthe at residing hole black supermassive the is A*) (Sgr A* Sagittarius sr-hH;atohsc;itreit-asbakhls observations; holes; black intermediate-mass astrophysics; astro-ph.HE; sr-hH;atohsc;osrain;SgtaisA;supermassive A*; Sagittarius observations; astrophysics; astro-ph.HE; o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW

117 oe esfrG science GW for News & Notes Notes & News for GW science 118 WNotes GW aeosraois igah fabnr fblack of binary death a to birth of from biography holes, gravitational A ground-based observatories: with wave IMBHs of Detection for issues key the cosmology. on to one evolution is stellar mass from into astronomy, their black of taking of branches of (not measurement many presence the magnitude the particular of Establishing in orders and holes). ten holes, black about primordial cover values hypothetic and of the our Range wide account in galaxies. is see well-developed masses can all we their of which centres of clusters, in and globular galaxies, in nearby galaxies, and nearby other in and Galaxy ytm.Sc eetoswudb rb oteselrevrnet fIMBHs of environments stellar the to these probe of a formation. existence their be the and would corroborate detections also Such would but with relativity, systems. us general provide of as only test high not robust as would a is observatories Mpc GW 100 ground-based at with for SNR acterization – the year 1000 and per and latter) 1000 (tens the – for promising 100 year more per much thousands becomes and or ﬁrst rate LIGO non-negligible. the event Advanced unfortunately, possibil- the as is, the ET, such and proposed glitch detectors, third-generation low the a and too with second- is to mistaken rate going are event When signals the Nevertheless, these that Mpc. ity 100 of that distance ﬁnd signal-to-noise a We a at with IMBHs frequencies. detecting of lower of (SNR) position to the ratio waveform in are the Virgo extend and LIGO numer- to initial with highest as the obtained so at model order calculations waveform post-Newtonian a available with on coupled based simulations of IMBHs relativity signal of ical the binary of a analysis of an present system We a (ET). Telescope LIGO, Einstein as future such the detectors and lower-frequencyVirgo ground-based in with chances astrophysics good (GW) has possibly, IMBH gravitational-wave and, an detection of of prospect characterization black The and observed. observation supermassive dra- was would IMBH of cosmography an and if evolution modeling change evolution matically and galaxy astro- as formation for well as interest of (SMBHs), high holes understanding of Our are objects these physics. observationally, corroborated been yet Abstract: parameter N-body; waveforms holes; dynamics; black stellar of estimation; binaries massive holes; black intermediate-mass Keywords: Eprint: Authors: http://arxiv.org/abs/0910.0254 mr-eae a;Snaai,Lucia Santamaria, Pau; Amaro-Seoane, vntog h xsec fitreit-asbakhlshsnot has holes black intermediate-mass of existence the though Even sr-hC;atop.A srpyis lblrcutr;GAEhw; GRAPE clusters; globular astrophysics; astro-ph.GA; astro-ph.CO; ∼ o tr itiueaon asv lc hole black massive a around distribute stars How 10 o ytm ihttlms ewe 0 and 100 between mass total with systems for 10 5 epciey h rset o MHdtcinadchar- and detection IMBH for prospects The respectively. a 1 2010 21, May 500 M

situated oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 Eprint: Authors: Loss Mass and Recoil Hole Black Disk to Gas Circumbinary a of Response Hydrodynamical Abstract: Keywords: Eprint: Authors: Schwarz- the in Geometry Orbits schild Circular for Self-Force itational Grav- the of Calculations Numerical and Post-Newtonian Keywords: needn eto h eydfeetrglrzto rcdrsivkdi h two an the provides in invoked it procedures schemes. particular, regularization The ap- approximation different In very both the well. of of systems. agree test soundness binary to independent the compact found confirms describing are comparison in calculation cultural proximations SF cross numerical this order the of first and through consistency ratio, result, from analytical mass out 3PN the The cancel to in order observable. proportional 3PN invariant poles the gauge the final at that the regularization show dimensional particle We in the appearing of regularization. 1/(d-3) self-field the dimensional divergent at the of evaluated regularize means and We particles by particles. point the (3PN) of two post-Newtonian one by of third generated location metric the the to involves up It pushed order. approximations. is different two calculation these using post-Newtonian system func- The the a of as frequency determined orbital the is of observable tion coordinate-invariant components particular the A for perturbative binary. m1/m2«1 The the ratio v. of mass velocities extreme orbital an small requires analysis for (SF) appropriate self-force most pow- is in and general expansion v/c«1, of in an ers involves techniques approximation approximation (PN) different post-Newtonian two The relativity. using addressed is orbits cular G)sucswudbigrc cetfi eet.Apoiigpsiiiy nthe in possibility, promising A benefits. scientific rich bring would sources (GW) holes Abstract: black supermassive holes; black of binaries massive kicks/recoil; parts; http://arxiv.org/abs/0910.0207 http://arxiv.org/abs/0910.0014 orls i . amn otn aFde,Andrew MacFadyen, Zoltán; Haiman, R.; Lia Corrales, F. Bernard Whiting, Le; Alexandre Tiec, Steven; Detweiler, Luc; Blanchet, h rbe facmatbnr ytmwoecmoet oeo cir- on move components whose system binary compact a of problem The idn lcrmgei E)cutrat fftr rvttoa wave gravitational future of counterparts (EM) electromagnetic Finding eea eaiiy rq;ps-etna hoy efforce self theory; post-Newtonian gr-qc; relativity; general crto ic;atop.O sr-hH;atohsc;E counter- EM astrophysics; astro-ph.HE; astro-ph.CO; discs; accretion o tr itiueaon asv lc hole black massive a around distribute stars How WNotes GW

119 oe esfrG science GW for News & Notes Notes & News for GW science 120 WNotes GW ikmyb eetbe eflo h otmre vlto fati,zero- thin, a of recoil of km/s 530 the evolution from a arising post-merger perturbations analyze We the that FLASH. hydro- the code follow using dynamic is simulations, We two-dimensional (SMBHB), with disk gas binary circumbinary detectable. viscosity hole circumbinary be supersonic black a may super-massive in disk disturbances a merger-induced from of emission coalescence prompt the of case bu 00k/.Eiso terirtmscnmil eutfo h epneof response the from result mainly can times earlier be at may Emission mechanism km/s. this 1000 to about due ( signature mass emission low prompt for A depending observable strongly vary angle. We to kick found the is estimates. which upon analytic curve, plane. light our disc bolometric verify the the to compute to also simulations and close difference simulations directed finite (SPH) is Hydrodynamics dimensional Particle recoil two Smooth the dimensional if three underestimate magnitude, use This of We en- loss. order kinetic energy real the an the only exceed underestimate include can gas, that circular- disc to the estimates, attempts by dimensional gained disc Thus, ergy en- outer the radii. of in smaller source gas at dominant as ize released the energy, that potential analytically often those is is show from ergy hole We significantly black differ investigations. recoiling results Our previous the if of disc. circumbinary results thin that black a merged dissipation, by the energy surrounded to the recoil consider substantial We a impart hole. can that waves, gravitational of sion Abstract: holes black supermassive Keywords: Eprint: Authors: light first the mergers: hole Black spiral the on effects major other any over- without the 15-20%, and pattern. by in overdensities shock disk loss shock the mass the of 5% reduces luminosity a mass-loss all in The results emission remnant. also wave We merger SMBHB. gravitational the central which the in of case luminosity the times Eddington analyze the few of reaches 10% and about months, to of sponding time-scale luminosity the The on light-curve. steadily disk post-merger rises the corresponding the that and estimate dissipation Assuming we of temperature, with disk. constant amount well collisionless a agrees maintain a to perturbations in instantaneously mass the nearly occur radiates of the to predicted evolution of caustics and 20% of morphology about those The up sweeping spiral disk. single-armed outward, the a propagates of that and find We forms wave gas. the shock for state of equation pseudo-isothermal 10 6 M

http://arxiv.org/abs/0910.0002 iay retdi h ln fteds,asmn ihra daai ra or adiabatic an either assuming disk, the of plane the in oriented binary, os,EeaM;Ldt,G;Amtg,P . rnl,J . ig .R. A. King, E.; J. Pringle, J.; P. Armitage, G.; Lodato, M.; Elena Rossi, h olsec fsprasv lc oebnre cusvateemis- the via occurs binaries hole black supermassive of coalescence The sr-hG;atop.E srpyis Mcutrat;kicks/recoil; counterparts; EM astrophysics; astro-ph.HE; astro-ph.GA; o tr itiueaon asv lc hole black massive a around distribute stars How 10 6 oa as lc oe hs eolvlcte exceed velocities recoil whose holes black mass) solar a 1 2010 21, May 10

r/,corre- erg/s, oe esfrG science GW for News & Notes Notes & News for GW science 3My2,2010 21, May #3 h ict h oso as stebakhlsmre edrv nltclythe analytically derive We merge. holes black the as happen. mass, to this of for loss condition the to disc the Abstract: Keywords: Eprint: rico radii Jacobi to Authors: half-mass their of ratio clus- the globular from Galactic ters of populations two for Evidence (mode- con- Regularisations is geodesic field. the Riemann-Hurwitz perturbations) latter, and the plus the self- (background of sum in the total part while approach, the back-scattered former geodesic, in the the background ceived tail, In the the upon function. via acts Green perturbations computed force radiative the a is of via star impact or the The perturbations, of in field. motion forward strong the step in giant on a gravitation constitute of will understanding holes black the supermassive by stars of capture Abstract: force self physics.hist-ph; Keywords: Eprint: holes Authors: black around stars of motion and Self-force rus n ru fcmat ial-nefiln lseswith clusters tidally-underfilling compact, of group one distances groups: galactocentric with clusters that radii show Jacobi their and clusters ular require the like trajectories motion, the non-adiabatic of The evolution approach. the self-consistent studying particle. for techniques the sophisticated of most the size infinitesimal the from ie n riso h lses eageta opc lsesadms lsesin clusters most and clusters compact relaxation that the argue on we Based clusters, groups population. the these halo of of younger orbits and or one times old to the cluster in particular membership its a and of have membership which the clusters between filling correlation tidally of group another http://arxiv.org/abs/0909.5696 http://arxiv.org/abs/0909.5558 plic,A;Aui,S. Aoudia, A.; Spallicci, amad,Hle;Prete,Gnvee ils ak eprn,En- Vesperini, Mark; Gieles, Genevieve; Parmentier, Holger; Baumgardt, hog eeto ylwgaiainlwv pc nefrmtr,the interferometers, space wave gravitational low by detection Through eivsiaetertobtentehl-asradii half-mass the between ratio the investigate We sr-hG;atohsc;goua lses tla dynamics stellar clusters; globular astrophysics; astro-ph.GA; sr-hH;ER;gnrlrltvt;goei oin rq;hep-th; gr-qc; motion; geodesic relativity; general EMRI; astro-ph.HE; o tr itiueaon asv lc hole black massive a around distribute stars How ζ ucin nevn ocne iegniscoming divergencies cancel to intervene function) r J ie yteptnilo h ik a and Way Milky the of potential the by given WNotes GW R GC 0 > . 1 8 < p alit w distinct two into fall kpc r h / r J r < h fGlci glob- Galactic of r 0 h / . 3 r efidno find We . J < 0 . 05 and

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