The dynamically hot stellar halo around NGC 3311: a small cluster-dominated central galaxy
aa r X i v : . [ a s t r o - ph . C O ] S e p Astronomy&Astrophysicsmanuscript no. gventimi c (cid:13)
ESO 2018November 20, 2018 L ETTER TO THE E DITOR
The dynamically hot stellar halo around NGC 3311: a smallcluster-dominated central galaxy ⋆ G. Ventimiglia , , O. Gerhard , M. Arnaboldi , , and L. Coccato Max-Plank-Institut f¨ur Extraterrestrische Physik, Giessenbachstra β e 1, D-85741 Garching bei M¨unchen, Germany. European Southern Observatory, Karl-Schwarzschild-Stra β e 2, 85748 Garching bei M¨unchen, Germany. INAF, Osservatorio Astronomico di Pino Torinese, I-10025 Pino Torinese, Italy.Received July 27, 2010; accepted September 10, 2010
ABSTRACT
Context.
An important open question is the relation between intracluster light and the halos of central galaxies in galaxy clusters.
Aims.
Here we report results from an on going project with the aim to characterize the dynamical state in the core of the Hydra I(Abell 1060) cluster around NGC 3311.
Methods.
We analyze deep long-slit absorption line spectra reaching out to ∼ kpc in the halo of NGC 3311. Results.
We find a very steep increase in the velocity dispersion profile from a central σ = 150 km s − to σ out ≃ km s − at R ≃ kpc. Farther out, to ∼ kpc, σ appears to be constant at this value, which is ∼ of the velocity dispersion of the HydraI galaxies. With its dynamically hot halo kinematics, NGC 3311 is unlike other normal early-type galaxies. Conclusions.
These results and the large amount of dark matter inferred from X-rays around NGC 3311 suggest that the stellar haloof this galaxy is dominated by the central intracluster stars of the cluster, and that the transition from predominantly galaxy-boundstars to cluster stars occurs in the radial range 4 to 12 kpc from the center of NGC 3311. We comment on the wide range of halokinematics observed in cluster central galaxies, depending on the evolutionary state of their host clusters.
Key words. galaxies:clusters:general – galaxies:clusters:individual (Hydra I) – galaxies:kinematics and dynamics – gal-axies:individual (NGC 3311)
1. Introduction
An important open question is the physical and evolutionaryrelation between the intracluster light (ICL) and the extendedhalo of the brightest cluster galaxies (BCGs), whether they aretruly independent components or whether the former is a radialextension of the latter. Using a sample of 683 SDSS clustersZibetti et al. (2005) found a surface brightness excess with re-spect to an inner R / profile that characterizes the mean profileof the BCGs, but it is not yet known whether this cD envelope issimply the central part of the cluster’s diffuse light component,or whether it is distinct from the ICL and part of the host galaxy(Gonzalez et al. 2005).In the Southern hemisphere, the cD galaxy NGC 3311 andthe giant elliptical NGC 3309 dominate the central region of theHydra I cluster, an X-ray bright, non-cooling flow, medium com-pact cluster with a velocity dispersion σ HydraI = 784 km s − (Misgeld et al. 2008). The X-ray observations show that the hotintracluster medium centered on NGC 3311 has a fairly uniformdistribution of temperature and metal abundance from a few kpcout to a radius of kpc (Tamura et al. 2000; Yamasaki et al.2002; Hayakawa et al. 2004, 2006). Given the overall regular X-ray emission and temperature profile, the Hydra I cluster is con-sidered as a prototype of an evolved and dynamically relaxed Send offprint requests to : G. Ventimiglia, e-mail: [email protected] ⋆ Based on observations collected at the European Organisation forAstronomical Research in the Southern Hemisphere, Chile, during theobserving program 082.A-0255(A) on 2009 March 25. cluster; it is therefore a suitable candidate for a dynamical studyof a relaxed extended stellar halo around a BCG.The primary goal of this work is to establish the dynamicalstate of the stellar halo of NGC 3311. We use long-slit spectrato uncover the kinematics in the halo region of NGC 3311 out to ∼ kpc from its center. In Sect. 2 we present observations withFORS2 at VLT and the GEMINI GMOS archive data, whichwe reanalyze. We describe the data reduction and the kinematicmeasurements in Sect. 3. The newly measured halo kinematicsand their implications are discussed in Sect. 4, and our conclu-sions are summarized in Sect. 5.We adopt a distance to NGC 3311 of Mpc (NED), equiv-alent to a distance modulus of . mag. Then ′′ correspondsto . kpc.
2. Observations and archive data
VLT FORS2 long slit spectra - The long-slit spectra were ob-tained during the nights of 2009 March 25-28, with FORS2 onVLT-UT1. The instrumental setup had a long-slit . ′′ wide and . ′ long, Grism 1400V+18, with instrumental dispersion of 0.64˚A pixel − and spectral resolution σ = 90 km s − , and a spatialresolution along the slit of . ′′ pixel − . The seeing during ob-servations ranged from . ′′ to . ′′ . The wavelength coverage ofthe spectra is from 4655 ˚A to 5965 ˚A, including absorption linesfrom H β , MgI ( λλ , , ˚A) and Fe I ( λλ , ˚A). We obtained eight spectra of 1800 sec each, for a total ex-posure time of 4 hrs. In the FORS2 observations, the long slit iscentered on the dwarf galaxy HCC 26 at α = 10 h m . s Fig. 1.
Optical DSS ′ × ′ image centered on NGC 3311 in theHydra I cluster. The relative positions of the GMOS slit ( . ′ ,blue line) and FORS2 slit ( . ′ , red line) are illustrated. Greenand yellow sections on the FORS2 slit indicate regions whereaverage spectra are extracted. The adjacent numbers specify theradial distances of their light-weighted mean positions from thecenter of NGC 3311. The center of the FORS2 slit coincideswith the position of the dwarf galaxy HCC 26 and is marked bya black circle. North is up and East to the left.and δ = − d m . s (J2000), with a position angle ofP.A.= ◦ ; HCC 26 is seen in projection onto the NGC 3311halo. The position of the FORS2 long slit is shown in Fig. 1. Itscenter is located at P.A.= ◦ with respect to NGC 3311, approx-imately along the major axis of the galaxy. Gemini GMOS-South long slit spectra - We use Geminiarchive long-slit spectra in the wavelength range from 3675 ˚A to6266 ˚A observed with the B600 grating, a dispersion of . ˚A pixel − , a spectral resolution of σ = 135 km s − , and aspatial scale of . ′′ pixel − ; a detailed description of the in-strumental setup is presented in Loubser et al. (2008). The see-ing was typically in the range from . ′′ to . ′′ . We target thesame absorption lines as for the FORS2 spectra, i.e. H β , MgI( λλ , , ˚A) and Fe I ( λλ , ˚A). The . ′′ wide and . ′ long Gemini slit is centered on NGC 3311, at α = 10 h m . s and δ = − d m . s (J2000), alongP.A. = ◦ , the direction of the galaxy major axis. Its position isshown in Fig. 1.
3. Data reductions
The data reduction of the FORS2 long slit spectra is carried outin
IRAF . After the standard operations of bias subtraction andflat-fielding, the spectra are registered, co-added and wavelengthcalibrated. The edges of the FORS2 slit reach well into sky re-gions, which are then used to interpolate the sky emission in theregions covered by the stellar spectra.In the low surface brightness regions, spectra are summedalong the spatial direction in order to produce one-dimensionalspectra with an adequate S/N ratio ( ≥ per ˚A). Four indepen-dent one-dimensional spectra are extracted along the slit wherethe light is dominated by the halo of NGC 3311; of these, twoare from regions north and two from regions south of HCC 26,respectively. We extract spectra from slit regions of ∼ ′′ × . ′′ Fig. 2.
Kinematic fits with PPXF of the spectra extracted at − ′′ (VLT FORS2) and at − ′′ (Gemini GMOS). In black we dis-play the galaxy spectra, in green the wavelength range excludedfrom the fit because of sky residuals, and in red the best-fit-broadened template model. All spectra are normalized to thevalue of the best-fit model at 5100 ˚A.and ∼ ′′ × . ′′ at distances of about and from thecenter of NGC 3311, and of ∼ ′′ × . ′′ and ∼ ′′ × . ′′ atcentral distances of about and . We properly mask thespectra of foreground stars in those areas.The data reduction for the GMOS long slit spectra is car-ried out independently here, also in IRAF and with the stan-dard tasks in the Gemini package. The procedure is describedin Loubser et al. (2008) for the wavelength calibration and back-ground subtraction; also in this case the edges of the slit are usedto interpolate the sky emission in the regions covered by the stel-lar continuum. Because our goal is to sample the kinematics wellinto the halo, the one-dimensional spectra for the absorption linemeasurements are summed along the slit direction so that a min-imum S/N ∼ per ˚A is obtained in each radial bin, out to aradial distance of about from the center of NGC 3311. Stellar kinematics - The stellar kinematics is measured fromthe extracted 1D spectra in the wavelength range 4800 ˚A < λ < ˚A, using both the “penalized pixel-fitting” method (PPXF,Cappellari & Emsellem (2004)) and the Fourier correlation quo-tient (FCQ) method (Bender 1990), in order to account for pos-sible systematic errors and template mismatch.In the PPXF method, stellar template stars from the MILESlibrary (Sanchez-Blazquez et al. 2007) are combined to fit theone-dimensional extracted spectra; the rotational velocity, thevelocity dispersion and Gauss-Hermite moments (e.g. Gerhard(1993)) are measured simultaneously. Fig. 2 shows two of theextracted spectra and the broadened templates fit by PPXF. In theFCQ method, the rotational velocity and velocity dispersion arederived for each extracted one-dimensional spectrum by assum-ing that the LOSVD is described by a Gaussian plus third- andfourth- order Gauss-Hermite functions. Before to the fitting pro-cedure the MILES template spectra are smoothed to the GMOSand FORS2 spectral resolution with the measured broadeningoffsets. While FCQ provides error estimates along with the mea-sured kinematics, errors for the PPXF kinematic parameters are
Fig. 3.
Major axis line-of-sight velocity and velocity dispersionprofiles for NGC 3311 (P.A. = 63 ◦ ). The open light blue tri-angles are the values published by Loubser et al. (2008), basedon Gemini-South GMOS data. The black asterisks are our inde-pendent measurements from these GMOS (archival) spectra, andthe red asterisks show measurements from the new VLT-FORS2spectra. These are weighted averages of three independent mea-surements which are obtained with PPXF and FCQ as describedin Sec. 3 and shown separately as the gray, magenta and greendiamonds. The FORS2 data points are obtained from averagesover ∼ ′′ and ∼ ′′ in the inner regions and over ∼ ′′ and ∼ ′′ in the outer regions of the slit; see Fig. 1. These off-axismeasurements are plotted at their light-weighted average radii,corrected for projection onto the major axis of NGC 3311 withan isophotal flattening of 0.89. Positive distances are south-westfrom the center of NGC 3311 and negative values are north-east,along P.A.= ◦ .calculated with a series of Monte Carlo simulations adopting theappropriate S/N for each bin.Because the stellar populations in cD halos may have differ-ent metal abundances and ages from those of the inner regions(Coccato et al. 2010a,b), systematic effects caused by templatemismatch must be evaluated and accounted for. We therefore ex-tract kinematic measurements with PPFX and FCQ as follows:1. fit with PPFX the best stellar template from the MILES li-brary in the central regions with the highest S/N, and extract v and σ at all radii, using the same stellar template;2. simultaneously fit the best stellar template, v and σ in eachradial bin with PPFX;3. adopt the respective best-fit PPXF stellar template to derivethe LOSVD with FCQ for all radial bins;4. finally, average rotational velocities v and velocity disper-sions σ are computed as weighted means of the three val-ues extracted in each radial bin as detailed above. Errorsfor these weighted average values are computed from thoseof the three measurements, but if the reduced χ = n − P ni =1 ( x i − ¯ x ) ǫ i is greater than one, they are increased by p χ in order to take into account systematic differences.I.e., ǫ x = P ni =1 /ǫ i × χ where ǫ i , ǫ ¯ x are the errors on theindividual measurements x i and the weighted mean ¯ x , re-spectively.Mean velocities and velocity dispersions in all radial binsare listed in Table 1, and the profiles are shown in Fig. 3together with the previous measurements from Loubser et al.(2008). Table 1, which is available in electronic form, containsthe following information: source of data (Col. 1), distance fromgalaxy center (Col. 2), P.A. (Col. 3), v , σ with errors for eachof the procedures 1.-4. described in the text, in Col. (4-5), (6-7),(8-9), and (10-11), respectively. Heliocentric and relativistic cor-rections have been applied to the mean velocities. The systemicvelocity is − and has been subtracted.In the central region of NGC 3311, our new velocity dis-persion profile marginally agrees with that of Loubser et al.(2008). The new mean line-of-sight velocity measurementsagree with the systemic velocity of NGC 3311 obtained byMisgeld et al. (2008), but have a systematic offset from the v data of Loubser et al. (2008), by about 91 km s − . The agree-ment between the new FORS2 measurements at − and therevised value at − from archive GMOS data gives us con-fidence that the systematic effects from wavelength calibrationoffsets, template mismatch, etc., are sufficiently small in the new,independent data reductions. However, several tests have con-vinced us that the data do not allow us to reliably determine fullline-of-sight distributions (e.g., h , h ), which could be used totest for subcomponents, which one would expect in particular atradii ∼ − .
4. The kinematics of the NGC 3311 stellar halo
The combined new velocity dispersion profile for NGC 3311reaches to R mj = 39 ′′ ≃ kpc from the center of NGC 3311along the galaxy’s major axis (P.A.= ◦ ), and to an off-axis dis-tance of R = 100 ′′ ≃ kpc along the FORS2 slit. It showsa very unusual steep rise with increasing radial distance fromthe galaxy center: from a central value σ = 150 km s − , to σ = 231 km s − at R = 15 ′′ ≃ . kpc, and then on toa flat σ out ≃ km s − outside R = 47 ′′ = 12 kpc. Thesteep outward gradient is supported by two independent data setsand data reductions. The measurements of Loubser et al. (2008)near the galaxy center had already hinted at a positive gradientfrom km s − at R = 5 ′′ to ∼ km s − at a radius of R = 10 ′′ , and data shown in Fig. 1 of Hau et al. (2004) reach ≃
300 km s − at ∼ . With the new data we now have veryclear evidence of a dynamically hot stellar halo in NGC 3311.To put the extremely rapid rise of the velocity dispersion pro-file of NGC 3311 in context, we compare its kinematic propertieswith those of early-type galaxy (ETG) halos mapped using plan-etary nebula data (Coccato et al. 2009) and with the halos of thetwo Coma BCG galaxies NGC 4889, NGC 4874 from deep ab-sorption line spectroscopy (Coccato et al. 2010a). Fig. 4 showsthe mean < V /σ > , X-ray luminosity, and total absolute B-bandmagnitude for these galaxies versus their outermost halo velocitydispersion. For NGC 3311, we use a bolometric X-ray luminos-ity within ′′ ≃ kpc, L X = 2 . × erg s − (basedon the flux in the 0.5-4.5 keV energy range from Yamasaki et al.(2002) and corrected to bolometric L X according to Table 1 ofO’Sullivan et al. (2001)), and the total extinction corrected B-band magnitude (12.22) from de Vaucouleurs et al. (1991). Forthe velocity dispersion of NGC 3311, we use the values at the Fig. 4.
Properties of the stellar halo of NGC 3311 compared withother early-type galaxy halos: mean < V /σ > ( upper panel ),total X-ray luminosity ( central panel ), and B-band total magni-tude (lower panel) against stellar velocity dispersion σ . Solid di-amond, circle, and square show the measured σ of NGC 3311 atthe center, ( ≃ . kpc), and ( ≃ kpc). Crosses showoutermost velocity dispersions from Coccato et al. (2009), andopen diamonds for NGC 4889/4874 from Coccato et al. (2010a).center, at ( ≃ . kpc) and at ′′ ( ≃ kpc). Only the cen-tral σ puts NGC 3311 in the middle of the ETG distribution; σ (47”) deviates strongly, with a much larger σ than expectedfor the given L X , B T .The natural interpretation for these results is that the outerstellar halo of NGC 3311 is dominated by the central intraclusterstar component of the Hydra cluster. This is supported by sev-eral pieces of evidence: (i) The steep rise of the σ -profile; moreisolated ETGs all have slightly or even steep falling σ -profiles(Coccato et al. 2009). (ii) The saturation of σ at ≃ kpc, out-side of which the dynamically hot component dominates com-pletely. σ (47”) is ∼ of the galaxy velocity dispersion inthe cluster core. (iii) The large amount of dark matter inferredfrom X-ray observations around NGC 3311 ( ∼ M ⊙ within20 kpc, Hayakawa et al. (2004)).In recent cosmological hydrodynamic simulations of clusterformation, Dolag et al. (2010) applied a kinematic decomposi-tion to the stellar particles around cD galaxies. With a doubleMaxwellian fit to the velocity histogram of star particles cen-tered on a simulated cD, they were able to separate an inner,colder Maxwellian distribution associated with the central gal-axy, and an outer, hotter component of stars that orbit in the clus-ter potential. For both components they derived radial densityprofiles and, fitting Sersic profiles, found that the inner stellarcomponent is much steeper than the outer diffuse stellar com-ponent. A comparison with these simulations indicates that the steep velocity dispersion gradient in the halo of NGC 3311 tracesthe transition from central galaxy stars to the diffuse intraclusterstellar component. In the NGC 3311 halo, the transition betweenthe two occurs at smaller radii than in other BCGs in nearby clus-ters, in the range between 4 and 12 kpc.NGC 3311 appears to have a similar halo as the cD galaxyNGC 6166 in the Abell 2199 cluster (Kelson et al. 2002), whose σ -profile rises to cluster values at R ∼ kpc. But NGC 3311is even more extreme; it is a fairly small galaxy, based on itscentral σ = 150 km s − , and it is already dominated by thesurrounding cluster component at R ∼ kpc. Presumably, thisis because the core of the “relaxed” Hydra cluster has had timeto collapse onto the galaxy. For comparison, the two BCG gal-axies in the Coma cluster core, which have a nearly constant σ -profile (Coccato et al. 2010a), may be in the middle of an on-going merger (Gerhard et al. 2007), so that their previous sub-cluster halos would have been stripped and a new cluster halocould have been built only after the merger was completed; andin the outer halo of the more isolated M87, the velocity disper-sion appears to drop (Doherty et al. 2009) towards the edge.
5. Conclusions
Based on two independent long-slit data sets and reductions, wefind a steep gradient in the velocity dispersion profile of the cen-tral galaxy NGC 3311 in the Hydra I cluster, from σ ≃ km s − to σ out ≃ km s − outside 12 kpc (60% of the ve-locity dispersion of the galaxies in the surrounding cluster).The new data provide evidence that NGC 3311 is a fairlysmall galaxy dominated by a large envelope of intracluster starsalready beyond R ∼ kpc, whose orbits are dominated by thecluster dark matter potential. Comparison with other BCG gal-axies shows a wide range of dynamical behavior in their halos. Acknowledgements.
The authors wish to thank the ESO VLT staff for their sup-port during the observations and the referee for a constructive report. This re-search has made use of the Gemini archive data, the NASA/IPAC ExtragalacticDatabase (NED), which is operated by the Jet Propulsion Laboratory, CaliforniaInstitute of Technology, under contract with the National Aeronautics and SpaceAdministration.
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Measured mean velocities and velocity dispersions for NGC 3311. For details see text. The galaxy’s systemic velocity V sys = 3800 km s − has been obtained by alinear fit to the velocities in the central ′′ and has then been subtracted from the measurements. This value includes heliocentric and relativistic corrections. Instr. R P.A. V ppxf1 σ ppxf1 V ppxf2 σ ppxf2 V FCQ σ FCQ < V > < σ > (arcsec) ( km s − ) ( km s − ) ( km s − ) ( km s − ) ( km s − ) ( km s − ) ( km s − ) ( km s − )(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)GMOS-S . ◦ ±
33 399 ± − ±
33 381 ± − ±
45 435 ± − ±
31 401 ± GMOS-S .
89 63 ◦ − ± ± − ± ± − ± ± − ±
11 235 ± GMOS-S .
88 63 ◦ − ± ± − ± ±
15 19 ± ± ±
12 195 ± GMOS-S . ◦ − ± ± − ± ±
13 1 ± ± − ± ± GMOS-S ◦ − ± ± − ± ± − ± ± − ± ± GMOS-S − .
09 63 ◦ ± ± − ± ±
14 16 ± ± ± ± GMOS-S − .
05 63 ◦ ±
11 244 ±
20 9 ±
11 200 ±
20 26 ± ± ± ± GMOS-S −
15 63 ◦ ±
11 295 ± − ±
11 267 ±
16 30 ± ± ±
11 231 ± GMOS-S −
34 63 ◦ ±
13 323 ±
22 50 ±
13 252 ± − ±
17 292 ±
18 60 ±
33 289 ± FORS2 −
47 45 ◦ ±
12 479 ±
14 71 ±
12 433 ±
14 117 ± ±
12 100 ±
15 460 ± FORS2 −
54 83 ◦ ±
13 456 ±
15 87 ±
13 447 ±
15 124 ± ±
14 105 ±
17 457 ± FORS2 −
67 6 ◦ ±
53 471 ±
49 66 ±
53 454 ±
49 97 ±
55 476 ±
97 83 ±
31 464 ± FORS2 −
100 114 ◦ ±
21 437 ±
35 47 ±
21 432 ±
35 50 ±
29 405 ±
51 35 ±
13 429 ± Notes – Col. 1: instrument. Col. 2: Radial distance from center of NGC 3311. Col. 3: Position angle of data with respect to NGC 3311’s center. Col. 4: Velocity measured with PPXF (usingtemplate determined at R = 0” ), relative to the galaxy systemic velocity. Col. 5: Velocity dispersion measured with PPXF (using template determined at R = 0” ). Col. 6: Velocity measuredwith PPXF (free template), relative to the galaxy systemic velocity. Col. 7: Velocity dispersion measured with PPXF (free template). Col. 8: Velocity measured with FCQ, relative to the galaxysystemic velocity. Col. 9: Velocity dispersion measured with FCQ. Col. 10: Weighted average velocity. Col. 11: Weighted average velocity dispersion.). Col. 6: Velocity measuredwith PPXF (free template), relative to the galaxy systemic velocity. Col. 7: Velocity dispersion measured with PPXF (free template). Col. 8: Velocity measured with FCQ, relative to the galaxysystemic velocity. Col. 9: Velocity dispersion measured with FCQ. Col. 10: Weighted average velocity. Col. 11: Weighted average velocity dispersion.