the missing goliaths slingshot - massive black hole recoil at m83

7/27/2019 The Missing Goliaths Slingshot - Massive Black Hole Recoil at M83

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The Astrophysical Journal Letters, 717:L42L46, 2010 July 1 doi:10.1088/2041-8205/717/1/L42

C 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A.

THE MISSING GOLIATHS SLINGSHOT: MASSIVE BLACK HOLE RECOIL AT M83

Horacio Dottori1, Ruben J. Daz2, Juan Facundo Albacete-Colombo3, and Damian Mast4,51 Instituto de Fsica, Universidade Federal do Rio Grande do Sul, Porto Alegre, Brazil; [email protected]

2 Gemini Observatory, AURA, Colina El Pino, La Serena, Chile; [email protected] Universidad Nacional del Comahue (CURZA), M. Esandi y Ayacucho S/N, Viedma CP 8500, Rio Negro, Argentina

4 Centro Astronomico Hispano Aleman, Calar Alto, (CSIC-MPG), Almera, Spain5 Instituto de Astrofsica de Andaluca-CSIC, C/Bajo de Huetor, 50, 18008 Granada, Spain

Received 2009 October 7; accepted 2010 May 13; published 2010 June 14

ABSTRACT

The FanaroffRiley II radio source J133658.3295105, which is also an X-ray source, appears to be projected ontothe disk of the barred-spiral galaxy M83 at about 60 from the galaxys optical nucleus. J133658.3295105 and itsradio lobes are aligned with the optical nucleus of M 83 and two other radio sources, neither of which are supernovaremnants or H ii regions. Due to this peculiar on-the-sky projection, J133658.3295105 was previously studiedby Gemini+GMOS optical spectroscopy, which marginally revealed the presence of H in emission receding at130 km s1 with respect to the optical nucleus. In this Letter, we reanalyze the Chandra spectroscopy carriedout in 2000. We show that J133658.3295105 presents an Fe K emission line at a redshift of z = 0.018. Thisredshift is compatible with a black hole at the distance of M 83. We discuss similarities to the recently reportedmicro-quasar in NGC 5408. This finding reinforces the kicked-off black hole scenario for J133658.3295105.

Key words: galaxies: evolution galaxies: individual (M 83) galaxies: kinematics and dynamics galaxies:

nuclei X-rays: individual (J 133658.3295105)

1. INTRODUCTION

The correlation between supermassive black hole (SMBH)mass and bulge velocity dispersion in spiral galaxies (Ferrarese& Merrit 2000; Gebhardt et al. 2000) points to a strong interplaybetween these systems in a hierarchical scenario of diskgalaxyformation (Okamoto et al. 2008). A paradigmatic outcome ofa merger of BHs is the recoil of the resulting BH (Bonninget al. 2007; Blecha & Loeb 2006) in response to the anisotropicemission of gravitational waves (Blecha & Loeb 2006). In a

triple BH system, the ejection of the smallest BH may happenfar in advance of the merger of the two largest objects (Iwasawaet al. 2006). There are two caveats to this scenario: the searchfor kicked-off BHs has been unsuccessful thus far (Bogdanovicet al. 2009), and supermassive binary BH systems, which shouldalso be common objects, are elusive (Boroson & Lauer 2009).

The source J133658.3295105 emits X-rays (Soria & Wu2003; XS39, sources from Soria & Wus list will be citedwith the list number preceded by XS) and is also resolved inradio (Maddox et al. 2006; RS28, sources from Maddox et al.will be cited with the list number preceded by RS). RS28 ischaracterized as a FanaroffRiley type II (FRII) radio source.In addition to a flat-spectrum radio core, RS28 also presentstwo distinct radio lobes clearly showing the effect of relativistic

boosting at 25

0.5 kpc northwest (RS27) and southeast(RS29) of the core. They are projected onto the disk of thebarredspiral M83 at about 60 (1.3 kpc) of thegalaxys opticalnucleus (ON). J133658.3295105 and the radio lobes presentan on-the-sky alignment with respect to the galaxy ON (Cowanet al. 1994) and the radio sources RS30 and RS32 (Dottoriet al. 2008a, 2008b). The ON of M83 itself is shifted fromthe galaxys kinematic center (KC; Thatte et al. 2000). Mergerprocesses (Diaz et al. 2006), as well as galactic inner buildup(Elmegreen et al. 1998), are now evident in M83. At a distanceof about 4.5 Mpc (Karachentsev et al. 2002), M83 belongs tothe Hydra-Centaurus group, one of the most active regions inthe nearby universe and recently detected as a source of ultra

high-energy cosmic rays (Abraham 2007). Soria & Wu (2003)proposed a distance of z 1, arguing that known FRII radiogalaxiesalways have a lowerlimit ofL6 cm andL20cm (Kembhavi& Narlikar 1999). Gemini+GMOS observations (Dottori et al.2008b; GS-2007A-DD-17) marginally detected H emissioncoming from J133658.3295105. This emission indicates areceding speed of 130 4 0 k m s1 with respect to the M83 ON.In this study, we critically analyze the detection of Fe K X-rayemission line in the X-ray counterpart of J133658.3295105(XS39).

2. CHANDRA X-RAY OBSERVATION

Of the three available X-ray observations of the M83 spiralgalaxy (one from XMM-Newton and two from Chandra), XS39was detected in the deepest Chandra observation on 2000 April29 (ObsID: 793). It is located 1 off-axis from the ACIS-S3aim point. The total exposure time was 50.981 ks. After screen-ing out observational intervals with strong background flares,a good time interval of 50.811 ks was retained. We hereafterassume a non-variable background. Data were acquired in theFAINT observation and TIMED read modes. Data reduction,starting with the Level 1 event list provided by the pipelineprocessing at the Chandra X-Ray Observatory, was performed

using the latest version of CIAO

6

(ver. 4.1.2) and the CALDB(ver. 4.1.3) set of calibration files. Photon energies were cor-rected for the time dependence of the energy gain using thecorr_tgain CIAO task. To avoid calibration uncertainties, theevent data were filtered on energy using the range 0.58.0 keV.

In Figure 1, we show the projected position of XS39 onthe disk of M83 in a false color combination of three X-raybandpasses plus a single H Gemini image. Before the color-coded image combination, we corrected the single-band X-rayimages for variations in exposures, sensitivity, and vignettingby computing and dividing with the respective exposure maps.

6 http://cxc.harvard.edu/ciao

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Figure 1. False four-color image of M83. The Chandra X-ray frames arecomposed of yellow (0.51.2keV), green(1.22.5 keV), and blue(2.58.0 keV)energies. The red image corresponds to the H image from the Gemini southtelescope. The Chandra ACIS-S image has been smoothed, and pixel intensitiesare displayed in a logarithmic scale. The inner panel of the figure shows that theX-ray emission of XS39 appears to be slightly elongated due to the local PSFof ACIS at the 1 off-axis angle. Note: the KC, ON, and hidden nucleus (HN)are indicated near the M83 core.

The hardness of the X-rays from XS39 is clear from Figure 1,indicating that most of the emission is in the 28 keV band.

2.1. X-ray Spectrum of J133658.3295105

The spectral data extraction was performed by following thestandard CIAO thread to extract an ACIS spectrum. The stepswere as follows: (1) extract source events within an ellipse ofsemi-axes 2.2 and 1.6 and a position angle of 150, mappingthe elongated local point-spread function (PSF) of the ACIS-Scamera at 1 (see Figure 1, inner panel); (2) create the aspecthistogram file; and (3) create the RMF and ARF files that areappropriate for the time-dependent source position on the chip.In addition to the standard thread, the event data were filtered

based on energy using the range 0.58.0 keV. The resulting netdetection of photons was 135. There was a net count rate of2.6 103 counts s1. To improve the signal-to-noise ratio(S/N) of the spectrum while avoiding excessive spectral reso-lution degradation, we binned the spectra to a minimum of twophotons perbin. Spectral fittingon theACISdata wascarriedoutwith the Interactive Spectral Interpretation System (ISIS; Houck& Denicola 2000). Because of the low photon statistic in theX-ray spectrum, the 2 statistic was avoided. Instead, we usedthe simplex minimization method and the Cash statistic (Cash1979).

By using the C-stat statistic and a pure blackbody or asingle power-law model to fit the X-ray spectrum of XS39, wefound that the residual contribution in the C-statistic regime, at

energies of the Fe K (6.7 keV) line complex, is around a factorof 40 or larger. This suggests that simple models are clearlyunrealistic in describing the X-ray spectrum of XS 39.

The XS39 X-ray spectrum (see Figure 2) is probably in-consistent with a pure blackbody or single power law. In theminimization procedure, we use a physical model that assumesthe presence of a thermal plasma in collision-filled ionizationequilibrium, as modeled by the apec code of Brickhouse et al.(2005). A Gaussian emission line is also assumed to fit the FeK complex (see Figure 2 for details).

The statistical significance of the Fe K line in a photon-limited spectrum is difficult to determine, even more so if it hasseven photons over the continuum, as in the case of the X-ray

Table 1

Spectral Fit Parameters

Model Parameters apec+gauss

apec

Nh (1022 cm2) 0.96 0.3

kT(keV) 7.7 1.9

Normalization 3.0 105

Abundance 1.0

FeK linePeak 6.52 0.04

Normalization 6.5 107

R (inout)

Inclination (deg)

Redshift 0.018+0.0060.007FluxFeK (cgs) 4 10

15

C -stat 0.69

Fluxx (cgs) 3.5 1014

Lx (erg s1) 5.6 1037

Notes. The model wasmultiplicativelyaffected by Galac-

tic absorption NH = 4.0 1020 cm2. Model normaliza-

tion is in units of photons s1 cm2 keV1. X-ray flux,

in units of erg s1 cm2, was computed in the 0.58 keV

energyrange. Ninety percent confidencelimitswere com-puted and expressed as error in the table. Note that by

using a two-thermal emission model, we also fit the

X-ray spectrum of the optical nucleus (ON). The com-

puted X-ray flux and luminosity of the ON were 1.6

1013 erg s1 cm2 and 2.62 1038 erg s1, respec-

tively. The Fe K line did not appear in the ON X-ray

spectrum.

spectrum of XS39. However, we can obtain an estimation by adirect comparison of the FeK line 2 residuals (see Figure 2,right panel). We study the residuals at the 6.7 keV energy bycomputing the C-stat residuals of a thermal (apec + gaussian)model that includes the K line with respect to a single apecmodel. We found that local residuals are about 0.3 and 7,

respectively. This implies that the inclusion of a Gaussian lineat the6.7 keV energy yieldsresiduals that are20 times smaller. Arobustresultin terms of the significance of the Fe K line cannotbe determined accurately because of the statistical comparisonbetween these two distributions. Otherwise, we were able tocompute the statistical confidence ranges of the emission lineby using the normalization parameter of the Gaussian fit. Asshown in Table 1, this line accounts for about 9% of the totalX-ray flux, i.e., 41015 erg s1 cm2. Theconfidence levels ofthe line can be computed from the Gaussian line normalization,i.e., gausssian.norm (6.5 107) parameter. We use the ISISconf task to compute the 90% confidence limit of the Fe Kline amplitude at 1.3 1063.6 107, which covers afactor of 50% in flux. However, the 99% confidence limit ranges

between 1.5 106 and 8.7 108, which isalmost an order ofmagnitude below the best-fit value. Hence, the fitted GaussianFe K line is 2.5 over the continuum level.

3. RESULTS

The models in Table 1 give a redshift of z = 0.018+0.0060.007.Within a 23 accuracy level of this determination, it is foundto be compatible with the receding velocity of 130 km s1 foundfrom the H emission line (Dottori et al. 2008b) and with thecurrently computed velocities of a kick-off (Blecha & Loeb2006). We remark that the Fe K (6.7 keV) clearly indicatesz 1.


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L44 DOTTORI ET AL. Vol. 717

105

104

103

0.0

1

Countss1k

eV1

J133658.3295105 (XS 39)

1016

1015

1014

F

(ergscm2s

1k

eV1)

521420

2

4

C

Energy (keV)

1015

1014

F

(e

rgscm2s

1k

eV1)

FeK6.7 keV residual for XS 39

APEC+Gaussian

APEC

5

0

5

C

Energy (keV)

Residual from APEC model

Residual APEC+Gauss model

Figure 2. Left: spectral photon energy distribution of the XS39 (upper panel). Unfolded X-ray spectrum appears in the middle panel. The spectrum is binned to aminimum of two photons per bin. C-statistic fit residuals appear in the bottom panel. Right: C-statistic residuals of the Fe K line (6.7 keV) for a model that includesa Gaussian line plus a thermal emission (APEC) or a model without line emission.

Figure 3 shows a blown-up portion of the Figure 1 field, alonga line through the ON and XS39, in which the X-ray sources aresuperimposed on a radio image. The astrometry of themaximumbrightness of XS39 and RS28 is shown in two-dimensionalcoordinates elsewhere (Dottori et al. 2008b, Figure 3). (, )agrees within 0.5 10 pc with the previous determinationsfor the two objects, namely, (13:36:58.39, 29:51:05.1) forXS39 (Soria & Wu 2003) and (13:36:58.34, 29:51:04.58) forRS28 (Maddox et al. 2006). The X-ray spectrum of XS39 isunique (Soria & Wu 2003) among the other 127 X-ray sourcesfound within an area of 12 12 centered at the nucleus ofM83. A circle with a radius of 0.5 is the upper limit for

the superposition area between the RS28 and XS39 positionerror circles. Therefore, an alignment by chance of a putativebackground radio galaxy (RS28) with XS39 will be proportionalto the area of this circle divided by the area covered by the

Chandra frame, which means 1:6 105. That makes thephysical association of RS28 and XS39 highly feasible, as notedby different authors (Stockdale et al. 2001; Soria & Wu 2003;Maddox et al. 2006).

At the distance of M83, the projected distance between theradio lobes of J133658.3295105 is about 1 kpc. As a matter ofcomparison, the distance between lobes in FRII radio sources,centered in nuclei of active galaxies and quasars (DRAGN7)covers a wide range of lengths, from a few tens of pc to sev-eral Mpc. There is nothing odd with the double-source sepa-

ration, but only with the location of the central source com-ing outward from the nuclear region. From this point of view,off-centered micro-quasars and the Ultra-Luminous X-RaySource (ULX) observed in the Milky Way and nearby galax-ies are more adequate reference objects. The recently detectedlargest extragalactic micro-quasar in NGC7793 has a lobe-to-lobe projected size of more than 250 pc (Soria et al. 2009).The authors consider this object as an analog of SS433. Con-trary to these micro-quasars, J133658.3295105 does not showsigns of a surrounding nebula, as SS433 does (W50 nebula),suggesting that J133658.3295105 is outside of the galactic

7 www.jb.man.ac.uk/atlas/index.html

Figure 3. Blow-up along the line through the optical nucleus and XS39. TheX-ray sources are shown in blue-white, the H emission in green, and the 6 cmradio emission in red. We detached the maxima of the radio sources along the

jet-like radio feature as well as the ON. XS39 and RS28 are the X-ray and radioidentifiers of J133658.3295105, respectively.

plane. This scenario is supported by the redshift derived fromthe H emission line (Dottori et al. 2008b).

If J133658.3295105 were similar to the active galacticnuclei (AGNs), the ratio log(F(X)/F(opt)) would be about1 (Mushotzky 2004). The X-ray flux quoted in Table 1 isF(0.28.0 keV) 3.5 1014 erg cm2 s1, which wouldcorrespond to an optical counterpart at the1819 maglevel. Thisis at least 3 mag brighter than the detection limit of the availableGMOS/Gemini-S imagery (Dottori et al. 2008b), which doesnot show such a bright optical counterpart. Indeed, from a direct
http://www.jb.man.ac.uk/atlas/index.htmlhttp://www.jb.man.ac.uk/atlas/index.html


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comparison with the observations, the authors estimate that theircomposed image could detect more than 80% of the broad andnarrow line AGNs at 1 z 3 in the SEXSI sample (Eckartet al. 2006), irrespective of the redshift. In agreement with Soria& Wu (2003) work, our analysis does notshow X-ray variability.

A recently studied micro-quasar in NGC5408 (Soria et al.2006) shows up at a B brightness mB 23 mag. A sim-ilar object could not have been detected in the above-mentioned Gemini imagery, but should easily be observed withlonger exposure times. The luminosity of this micro-quasar islog(LH) 36.18(Soriaet al. 2006), which compares well withJ133658.3295105s luminosity of log (LH) 36.1 0.15.Both sources are log(LH) 0.5 fainter than the lower limitof the H luminosity function obtained from 17.797 extragalac-tic H ii regions (Bradley et al. 2006). This strongly suggeststhat a mechanism that is different from that of ionizing stars isresponsible for the H excitation in these objects.

Ascarriedoutby Laor& Behar (2008) for radio-quiet quasars,we obtained the RX relation. To calculate LR = L(6 cm),we use, for RS28, f(6 cm) = 0.87 mJy (Maddox et al. 2006,1998 observations) from the nearest date to that of the Chandraobservation. We obtained LR = 1.5 10

36 erg s1. The X-

ray luminosity was calculated by the direct integration of thelaw presented in Table 1, yielding LX = 1.1 1038 erg s1.

Then, the RX relation is log(LR/LX(0.220 keV)) 0.01,which is 2 orders of magnitude larger than the mean relation,log(LR/LX(0.220 keV)) 10

5, which fits cool stars, ULX,Seyfert nuclei, and radio-quiet quasars over an interval ofmore than 15 decades in X-ray luminosity (Laor & Behar2008). Although LR compares well with the interval of radioluminosities between ULX and Seyfert nuclei in Laor & Behar(2008, Figure 3), the X-ray luminosity of J133658.3295105is approximately 2 orders of magnitude fainter than the faintestULX source presented by the authors.

With respect to other space observations of M83, unfortu-nately, Hubble Space Telescope images do not cover the region

of J133658.3295105. Spitzer images at 5.8 m and 8 mbands with exposure times of 220 s and 210 s and brightnesslimits of 6.77 Jy and 12.95 Jy at (S/N) = 3, respectively, donot show an infrared counterpart at the object position.

4. DISCUSSION

The morphology of the radio emission distribution thatprotrudes along a line joining the ON of M 83 andJ133658.3295105 suggests that the quasar-likeobject has beenejected from the ON, which is off-set with respect to the galaxykinematical center. In that sense, it resembles the jet associ-ated with the quasi-stellar object (QSO) PKS112714.5 whichis also off-centered with respect to the QSO center (Siemigi-nowska et al. 2002). Nevertheless, the jet PKS112714.5 does

not include an FRII radio source, as the one associated withJ133658.3295105.

An ejected BH may drag its accretion disk together andaccrete interstellar matter during the transit through the bulgeand the densest part of the disk (Volontieri 2007). If the lurkingBH does not accrete fresh gas (argument suggested by thereferee), it will be seen as an AGN as long as the accretion diskremains reasonably full. Radio-loud AGNs may occur at lowerEddington rates, perhaps implying that the disk is emptying out.For a lifetime of 10 Myr, the source moved at least 1.3 kpcaway from the nucleus, which implies a transverse velocity onthe order of 100 km s1. That velocity is comparable with themeasured radial velocity for J133658.3295105 and compatible

with predicted kick-off ejection velocities, which run from a fewhundred to a few thousand km s1 (Bonning et al. 2007; Blecha& Loeb 2006). The composed velocity is relatively small and theobject would probably remain orbiting inside the galaxy untilit decays back to the center, according to Fujitas model (Fujita2009). In this case, the ejected BH will periodically accrete gasand its feeding will depend on its velocity as well as on thedensity and velocity dispersion of the interstellar medium thathas been crossed by the object (Volontieri 2007).

Further insight can be obtained from Fujita (2009, andreferences therein). These models contemplate the ejection ofan SMBH from the nucleus of a galaxy with bulge, disk,and halo components that are adequate for the Galaxy, witha circular velocity of 220 km s1 at R = 7 kpc. Fujita assumesChandrasekar dynamical friction, which makes the BH orbitdecay back to the center. Most of Fujitas simulations assumethat 20% of the disk is composed of gas, and that it is accretedinto the SMBH according to the BondiHoyle mechanism. TheX-ray luminosity of the SMBH is proportional to the accretionrate, to which an efficiency of about 10% is applied.

We take Fujitas models A1 and C3 and his Figures 7 and 9,respectively, as an example. The SMBH is launched from the

nucleus, at 500 km s

1

and 700 km s

1

in the (X,Z) plane, withan inclination of 30 with respect to the galactic plane. ModelA1 BH has 3 106 M. The dynamical friction time (tdf),defined as the time that it takes the SMBH to decay to an orbitof a maximum radius of 10 pc, is tdf = 0.63 Gyr. During thefirst 60 million years, the SMBH radiatesLX = 110

380.5 ergs1 at 14 and 44 Myr over periods of approximately 24 Myr.The relative velocity of the SMBH with respect to the disk ison the order of 250 km s1 and its height with respect to thedisk is around 0.1 kpc. Model C3 has an MSMBH = 3 10

7 Mand tdf = 3.7 Gyr. During the first 60 Myr, the SMBH radiatesLX = 1 10

380.5 erg s1 at 10 and 50 Myr during periodsof approximately 1020 Myr. In Model C3 the velocity withrespect to the disk is between 250 and 300 km s1, and its

height with respect to the disk is between 0.7 kpc and 1 kpc.The probability of observing the more massive BH is 5 timeshigher, which point to Fujitas model C3 as more appropriatedto describe the observed properties of J133658.3295105.

5. CONCLUDING REMARKS

The Chandra X-rays spectrum of J133658.3295105, asource projected on the body of M 83, presents Fe K lineat S/N 2.5 whose redshift (z 1) is compatible with thatobtained from the H emission line (620 km s1); both point toan object most likely located at the distance of M83.

Comparisons in the previous section (low X-ray lu-minosity, beaming, no surrounding nebulae) indicate thatJ133658.3295105 is not likely to be a ULX, but still

presents striking similarities to the micro-quasar in NGC5408.These similarities include the H luminosity (log (LH) 36.1 0.15) and the very faint or absent B-band brightness(mB > 22.5 mag).

The range of masses that are suggested by Dottori et al.(2008b) on a very simple basis is around 10 3104 solar masses,but intermediate-mass BHs may have much higher luminosities(Farret et al. 2009). This makes one more inclined to accept therange of masses derived from the Fujita models for kicked-off BHs (MBH 10

6107 M), based on a more coherenttheoretical scenario. Fujitas models with kick-off velocities of300 km s1 or smaller with respect to the galactic disk are morecompatible with our results.


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Longer integration times would be necessary to achievea higher S/N to define the Fe K line profile better andgain deeper insight into the physical characteristics of theJ133658.3295105 BH. This source may constitute the firstdetection of a kicked-off BH produced in a galactic nucleus.

The authors acknowledge the anonymous referee for help-ful suggestions. J.F.A.C. is a research member of the Con-

sejo Nacional de Investigaciones Cientficas y Tecnologicas(CONICET). H.D., R.D., and D.M. acknowledge the support ofMINCYT from Argentina and CAPES from Brazil. The GeminiObservatory is operated by the Association of Universities forResearch in Astronomy, Inc., under a cooperative agreementwith the NSF on behalf of the Gemini partnership, consisting ofthe NSF (USA), STFC (UK), NRC (Canada), ARC (Australia),MINCYT (Argentina), CNPq (Brazil) and CONICYT (Chile).

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