PoS(10th EVN Symposium)031 30 ∼ ies is within http://pos.sissa.it/ optical telescope ents and extended emission nsity and polarization maps ge optical emission” suggest a merger is questionable, and lable for the formation of RC VLBI and the new generation of radio nd show the presence of extended y asymmetric, with values of f 4.514, is one of the most luminous appears to be a core. The flux density in a timescale of less 1 Gyr appears to 196140, Russia ⊙ K11 9DL, U.K. 69167, Russia M 9 ) Black Hole (BH). Assuming that the age of the Universe ⊙ , A.I. Kopylov, O.V. Verkhodanov, T.A. Fatkhullin e Commons Attribution-NonCommercial-ShareAlike Licence. M ∗ 9 1.3 Gyr and that the standard epoch for the formation of galax ∼ 10 at 1.7 GHz. New optical observations using the Russian 6-m ∼ emission. The very high radio luminosities and the high “bul [email protected] (N.S. Soboleva) [email protected] (P. Thomasson) [email protected] (O.P. Zhelenkova) α RC J0311+0507, the parent galaxy of which has a redshift, z, o objects in the High-z radioof Universe. the New object MERLIN at and 1.7 GHz EVNorientated and in inte a 5 GHz primarily NS show direction multiple onratio compact either side between compon of the what southern and northern components is highl at 5 GHz and be very improbable. Speaker. the redshift range fromJ0311+0507. 7 The to quick 10, growth of there athe is BH simple less mass evolution from solely than several as 0.5 solar a masses result Gyr to of avai 10 the presence of a very massive (10 at z = 4.514 is only confirm the identification of theLy radio source with a galaxy, a ∗ Copyright owned by the author(s) under the terms of the Creativ c E-mail: N.S. Soboleva, A.V. Temirova SPb Branch of SAO RAS, Pulkovskoe sh., 65, Saint Petersburg, E-mail: P. Thomasson, T.W.B. Muxlow, R. Beswick The University of Manchester, JBO, Macclesfield, Cheshire S Special Astrophysical Observatory of RAS, NiznijE-mail: Arkhyz, 3

arrays September 20-24, 2010 Manchester UK 10th European VLBI Network Symposium and EVN Users Meeting: Yu.N. Parijskij, O.P. Zhelenkova MERLIN and EVN Observations of aGalaxy, RC z=4.514 J0311+0507, Radio and the problemin of the SMBH's Early Universe PoS(10th EVN Symposium)031 ) α at a ν α ∝ S Ly ian 6-m op- Fig. 1, right). d features, did otspots as part O.P. Zhelenkova ore of the radio = -1.31 ( t 1425 MHz sug- at 1425 MHz and hed version of the α ly the host galaxy, ′′ determinable and a ) ussian 6-m telescope project (RATAN-600 ompact steep spectrum nly known object close as based on the earlier vide the spectral index in- and 0.5 rvations with the SINFONI ndidate USS, FRII [10] radio GHz (left) and MERLIN 5 GHz ′′ , respectively. ′′ x 0.039 ′′ 2 and 0.110 ′′ x 0.132 object in R band. This emission line was identified with ′′ m The z=4.514 radio galaxy, RC J0311+0507, images: MERLIN 1.7 RC J0311+0507 was recognized as having an Ultra Steep Spectrum (USS RC J0311+0507 was imaged with MERLIN at 1.7 GHz (Fig. 1, left) and 5 GHz ( A more complex structureemission was still seen unidentifiable. than inof The earlier a nature observations, double-double of but structure with theMERLIN + or the compact VLA knots c image, components, showing along whether more jets h clearly in both the the compact source, and were more extende also in 1. Introduction between 365 MHz and 4850 MHz inas the the early stages finding of the survey “Bigtical instrument, Trio” survey telescope the VLA for as photometryRATAN-600 the 1980 and imaging “Cold” spectroscopy) radio instrument, [1 survey – and 5].catalogue at the derived 7.6 from Russ cm This the [6 UTRAO – survey survey 8]. at w formation 365 and An MHz a [9] initially necessary helped unpublis to better pro positionto for the the position VLA of observations. RC Thegested J0311+0507 an o was unequal double 4C+04.11, structure and and the agalaxy. object was first classified Further VLA as observations a image ca with of the it VLA a [2] at resolutions of 4.5 redshift of z = 4.514 [1].spectrograph This installed redshift on UT4 was of recently the confirmed VLT by [11]. obse 2. Radio and optical observations (right) with restoring beams 0.264 4860 MHz respectively showed an asymmetrical(CSS) double object. structure Optical for photometric this and c showed spectroscopic observations the with presence the R ofwhich a was strong observable emission as a line 23 at 6703Å in what was possib Figure 1: MERLIN and EVN Observations of a z=4.514 Radio Galaxy PoS(10th EVN Symposium)031 , s 30 ∼ 966 using . en for = -2.4. 47 α m larization is fields for all 11 10%). These h ” jet pointing 3 ∼ O.P. Zhelenkova tions in broad I tion of the radio at in the “bridge he fields are also = 4. The reduction an FRII structure, est with ss of the total flux n components ( region of weak, but t component 3 is or from us. mponents have been g to the south which e the core. However, 12% (25% and 8.6% (including the Lovell 2000 J -Band ( om an image obtained uld arise if it is moving ∼ & 2). This could be the the structure, which are α minates over a turbulent gion. Immediately prior fact that the polarization : aday rotation. There is no gth if this region is on the far ) appears to be approximately the ′′ 2.7 = -0.8, which is much flatter than the ∼ α 3 at 1.7 GHz were undertaken (Fig. 2). ′′ 0.4 and 1 mG have been found. These are quite strong fields, ∼ seeing conditions (Fig. 3, left). All the R-band available observa- ′′ to 1.5 ′′ 10 at 1.7 GHz). In fact, these are close to the extreme of what has been se ∼ The MERLIN and e-VLBI L-Band images clearly show that the source has Following the initial MERLIN observations and results, new optical observa This might be expected from the overall structure, with a southern “beamed The southern hot-spot regions show a mean polarization at 5 GHz of but with a very high asymmetry in the flux densities of the northern and souther The most compact (3),value has of the -1.31 for flattest the spectrumcontains integrated the with spectrum. nuclear source This or core. would The appear measured to position confirm of this tha core is tions (4 separate epochs) were used to improve the astrometry. 3. Results and middle SED 665 filtersSCORPIO [12] were with made 1.2 with the 6-m telescope in a direct imaging mode towards us and no jet visibleit to could the north be of that componentdensity 3, any of which polarization the appears two to is components. b barelycalculated, Where detectable all possible of the because spectral which of indices appear the of to the weakne be co steep, with component 1 being the steep MERLIN and EVN Observations of a z=4.514 Radio Galaxy not clarify the situation. Consequently,telescope) MERLIN with a and resolution e-VLBI of observations 0.025 greater than would be expectedin from polarization CMB at the radiation lower magnetic frequencymeasured fields polarization is at in probably the z caused northern = by 4.51 lobe greaterresult / of hot-spot Far increased region Faraday (components rotation 1 arisingside from an of increased the path source len from us. which will reduce the life-time of the high energy electrons in the components. T for components 7 and 8 respectively), with somewhat less polarization at L values are typical forangles the do hot-spot not change regions appreciably in indicatesone, that FRII a which radio regular limits magnetic sources. any field “internal” do region” rotation The in measure. the Further MERLIN evidencenot for 1.7 GHz too this image is dissimilar. th (Fig. Using 1, valuessolely from of left). the the EVN component data, The it angular positionthe is sizes possible components. angle derived to of fr Values make between estimates the of po “equipartition” magnetic same as that of the opticallysource visible relative galaxy, to but us this is could such be that illusory it if is the pointing orienta almost directly towards or away radio galaxies. There appear to benumbered 8 in small-sized, Fig. individual components 2. in Therefollows is a a highly jet curved from path, anto particularly unresolved the as component southern it (3) hotspots pointin approaches (7extended the & emission hotspot at 8), the re the noise level jet ofthrough appears the a image. to cluster The be curvature medium. on of The the the extent jet outer co of edge the radio of source a ( at 5 GHz and PoS(10th EVN Symposium)031 . , s ′′ 008 . 0 x 0.035 ± ′′ s nt (3) can be 966 eater than that O.P. Zhelenkova . redshift with a 1, at a redshift s galaxy at these 47 antly from normal teeper spectral in- m ut this also appears the spectral indices om the jet / hot-spot erably bent. All com- 11 lack of measured po- aday rotation, but if it onsequently, at shorter h that the direction of the 03 . This is a small fraction 1 = − two radio galaxies (including Hz · 2000 J α W 26 A MERLIN and e-VLBI 1.7 GHz com- 10 · 5 ∼ Figure 2: bined image with a restoring beam of 0.035 4 . ′′ 16 . 0 ± . This is in remarkable agreement with the optical position obtained from ′′ ′′ 79 87 . . 03 03 ′ ′ line radiation, probably arising 08 08 ◦ ◦ 2.2. Both have highly asymmetric α ∼ 05 05 Ly =+ =+ RC J0311+0507 is clearly one of the most powerful radio galaxies at high The MERLIN and EVN observations have The sizes of the I and SED 665 images are 1%) of the integrated radio luminosity at 5 GHz, which does not differ signific 2000 2000 J J ∼ radio luminosity equaling thatz = 5.19 of [15] the at the most sameTN J0924-2201) frequency distant with (see such radio [14]). high In galaxy, radio fact,dices there luminosity TN than J0924-220 RC are at J0311+0507 only z and > have equal 3,centimetre luminosities both wavelengths, at of 400 the MHz which [15] have radio .of s luminosity C TN J0924-2201 of because RC of J0311+0507wavelengths. its is “flatter” a A spectrum, factor making value it 2 forobtained the the from gr most the monochromatic luminou MERLIN luminosity map for at the 5 GHz, nuclear which compone is a weighted mean of the R-band images of the galaxy, which is: values for radio galaxies, but is smaller than would be expected for QSOs. ( definitely greater than thetion, indicating point that spread the parent func- opticala object galaxy is and notter, a the size QSO. of In the the objectthe is other SED 665 filters greater (Fig. than fil- 3, that left) in hydrogen because of intense ponents in the sources appearincreasing with to distance have steep from spectra, thelarization in with source the centres. the northern magnitudes lobe As of is, of indicated RC this J0311+0507 above, is may the also not found bestructure for caused in the by the component Far image on of themagnetic 1138-262. opposite field Likewise, is side one along of cannot the theto direction say nucleus be of for fr the the certain case jet as because for of 1138-262. orientation effects, b flux density distributions, with the visible jet / hot-spot structure being consid demonstrated that RC J0311+0507 is not aple sim- double, or abut has a double-double multi-component structure, radio each com- galaxy, ponent having a very high luminosity. Itsture struc- appears to be similargalaxy, 1138-262, to observed by that Pentericci of et al., the1997 radio- [13], but the latter has a significantlyredshift lower of 4. Discussion from gas surrounding the radio galaxy. δ MERLIN and EVN Observations of a z=4.514 Radio Galaxy δ PoS(10th EVN Symposium)031 , ⊙ M 10 , and BH ssibilities: tot use the flux before field P in the parent , m f the galaxy is ⊙ O.P. Zhelenkova photometry, the tween BH mass 22 M ter then 10 9 0.5 Gyr. However, nown. However, an f formation of field ∼ J0311+0507 has not olution from several xies. Even assuming (3, right), but includ- formation of an object ccretion theory would the Hubble Ultra-Deep than 0.3 – 0.1 Gyr, if the then 10 d to be ontours) in two wide (R and I) le) of RC J0311+0507 BH mass from ours (magenta) of the 5 GHz combined . The alternative is an unusual mechanism ⊙ M 3 have been suggested by Wang et al., 2007 [19]. 5 ⊙ 1.3 Gyr. Assuming a standard epoch of galaxy for- M at 5 GHz and BH mass. ∼ 5 tot P – 10 3 in less than a 1 Gyr time scale looks very improbable. In fact, primordial ) the high total and core radio luminosities and the high bulge optical emis- ⊙ 5 . M 2 BH 10 M ∝ tot 0.3 Gyr, the parent galaxy must be formed very quickly. There are two po P ∼ Left: the RC J0311+0507 images (grayscale images with blue c According to the well known correlations between integrated radio luminosities black holes with masses of at least 10 The age of the Universe at z = 4.514 is only and two middle (SED 665MERLIN and and SED VLA 707) map. filters Right:the with correlation an overlaid [16] estimation cont between (marked total by luminosity a red circ solar masses to 10 for the development of black holes in the early Universe, since the simple ev galaxy nucleus. Although thelocated MERLIN within and component EVN 3, the imagedensity mass indicates of of that the the the “flat-spectrum” BH core component isestimation within difficult o of to this the estimate core BH from region mass is this canand beca as be the yet made 5 from unk GHz the total “remarkably radio tighting emission correlation” as RC be J0311+0507 shown by (marked [17]. by Reproducing the their red plot circle), its BH mass is seen to be grea which is close to theindicate a present primordial day BH mass record. much greater Accepting than 10 this value, standard a Figure 3: MERLIN and EVN Observations of a z=4.514 Radio Galaxy mass [17], ( sion [18] suggest the presence of a very massive BH with a mass greater IR data are required to improveyet these been estimates. measured, but The using “dynamical the age”Field mean for [20] dynamical RC for ages z for = 4.514, field the galaxiesgiant age in elliptical of were the formed parent by galaxy a isan “merging expected age tree” to process of be from less small field gala mation to be at a redshift of 7–10, then less than 0.5 Gyr are available for the with such an extremely high radio“nuclear luminosity age” as of RC the J0311+0507. parent galaxy From of the RC BVRI J0311+0507 has been estimate galaxies, or the independentgalaxies. formation of a SMBH long before the epoch o independent early formation of giant stellar systems with absolute magnitudes - PoS(10th EVN Symposium)031 at f a , , h –4 h (85) laxy, RC 58 , lained by ir- nt Cold-80” at 365 MHz (723) 2000. O.P. Zhelenkova terval 22 ◦ PAZh udy of distant 5 , . s in the early 26 ies. The age of the , e of the short time to resolve problem. ossible that nuclear 71 rches 08–02–4863a, riod. Double core or (5) 1996. onent, very powerful < r galaxies or from col- AstL 40 δ , , igh luminosity RGs with < gths in the Early Universe. 3.5 ◦ ∼ 5 . BSAO >1.1) radio source sample - VLA , 35 α − ) optical data in all possible spectral ′′ 1 . , (673) 1992. 6 69 0.5 Gyr, but the nature and age of the parent galaxy , ∼ AZh , (433) 2006. 32 , (583) 1992. (297) 2000. 96 AstL 19 , , , A&AS The RATAN-600 7.6 cm catalogue of radio sources within the in The RATAN-600 7.6 cm catalog of radio sources from “Experime Investigation of RATAN-600 RC radio sources RATAN-600–VLA–BTA-6m (“Big Trio”) project: Multicolor st RC J0105+0501: A Radio Galaxy with Redshift z A&AT , RC J0311+0507: A candidate for superpowerful radio galaxie The Texas Survey of Radio Sources Covering , A deep sky survey at 7.6 cm with the RATAN-600 radio telescope Investigation of the RATAN-600 steep-spectrum ( in R, I) observations would provide a direct confirmation of the existence o m (1) 1991. (1945) 1996. 87 , 111 , declination of SS433 A&AS universe at redshift z = 4.51 1981. AJ FRII radio galaxies observations and optical identifications This work was supported by grants of the Russian Funds of Basic Resea Multi-component radio structures for low luminosity objects can usually be exp New MERLIN and EVN data have shown the complex structure of the radio ga [9] J.N. Douglas et al., [8] Yu.N. Parijskij et al., [1] A.I. Kopylov et al., [7] Yu.N. Parijskij et al., [2] W.M. Goss et al., [6] A.B. Berlin et al., [5] N.S. Soboleva et al., [3] Yu.N. Parijskij et al., [4] Yu.N. Parijskij et al., 07–02–12055ofi, 09–02–12169ofn, 10–07–00412a. References cluster of galaxies at such an early epoch. Acknowledgments bands. Deep (>25 MERLIN and EVN Observations of a z=4.514 Radio Galaxy may be better understood if there were high resolution (0 J0311+0507, the most powerful yet knownThe at precise short nature centimetre wavelen ofsource the activity has small been size stimulated by sub-components multi-mergingparent is effects galaxy in not has a been cluster clear, of estimated but galax to it be only is p regular “cooling flows” or by “largecomplex molecular structures and cloud” high accretions BH [15]. masseslisions H could between result two from SMBHs, mergers of seeradio cluste [21, galaxies, 22]. the However, for usual young,scale “multi-merging” for multi-comp explanation nuclear events seems - difficult smallerdouble becaus SMBH than variants, the discussed free-fall recently time in or Liu galaxy & rotation Wu (2002) pe [23] may help 5. Conclusion PoS(10th EVN Symposium)031 , , , 661 ion , , PAZh 297 (L48) Nature , , 4–6 in , ApJ ∼ , 388 w , MNRAS (67) 2008. O.P. 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