A&A 475, 497-506 (2007)
DOI: 10.1051/0004-6361:20078317

The innermost region of the water megamaser radio galaxy 3C 403

A. Tarchi1,2 - A. Brunthaler3 - C. Henkel3 - K. M. Menten3 - J. Braatz4 - A. Weiß3,5


1 - INAF-Osservatorio Astronomico di Cagliari, Loc. Poggio dei Pini, Strada 54, 09012 Capoterra (CA), Italy
2 - INAF - Istituto di Radioastronomia, via Gobetti 101, 40129 Bologna, Italy
3 - Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
4 - National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA
5 - IRAM, Avenida Divina Pastora 7, 18012 Granada, Spain

Received 19 July 2007 / Accepted 18 September 2007

Abstract
Context. The standard unified scheme of active galactic nuclei requires the presence of high column densities of gas and dust potentially obscuring the central engine. So far, few direct subarcsecond resolution studies of this material have been performed toward radio galaxies.
Aims. The goal of this paper is to elucidate the nuclear environment of the prototypical X-shaped Fanaroff-Riley type II radio galaxy 3C 403, the only powerful radio galaxy known to host an H2O megamaser.
Methods. Very Large Array A-array and single-dish Green Bank and Effelsberg 1.3 cm measurements were performed to locate and monitor the water maser emission. Very Long Baseline Interferometry 6 cm continuum observations were taken to analyze the spatial structure of the nuclear environment at even smaller scales, while the CO J = 1-0 and 2-1 transitions were observed with the IRAM 30-m telescope to search for thermal emission from a spatially extended, moderately dense gas component.
Results. Positions of the H2O maser features and the continuum emission from the core coincide within 5 mas (5.5 pc). Intensities of the two main maser components with (isotropic) luminosities sometimes surpassing 1000 $L{_\odot}$ appear to be anti-correlated, with typical timescales for strong variations of one year. If the variations are intrinsic to the cloud(s), the implied angular source size would be $\la$0.3 mas and the brightness temperature $\ga$5$\times $108 K. The VLBI continuum observations support a scenario where a nuclear core, represented by the dominant central radio continuum component, is accompanied by a jet and counterjet, directed toward the western and eastern large scale lobes of the galaxy. CO remains undetected, providing a maximum scale size of $\sim $50 pc $\times $ (500 K/ $T_{\rm b})^{1/2}$, with $T_{\rm b}$ denoting the brightness temperature of the CO J = 1-0 line. Possible scenarios that could produce the observed maser emission are outlined. Adopting a mass of several 108 for the nuclear engine, the observed maser features can only be interpreted in terms of an accretion disk as in NGC 4258, if they solely represent the systemic velocity components. The receding and approaching parts of the putative maser disk are, however, not seen and a secular velocity drift of the observed features is not (yet) apparent. Most likely, the two main maser components mark shocked molecular gas interacting with the nuclear jets. The X-shaped morphology of the radio galaxy may point at a binary nuclear engine. This possibility, greatly complicating the nuclear environment of 3C 403, should motivate a number of worthwhile follow-up studies.

Key words: galaxies: individual: 3C 403 - galaxies: active - galaxies: ISM - radio lines: ISM - radio lines: galaxies

1 Introduction

The physical conditions in active galactic nuclei (AGN) are unique in the cosmos. Stellar and gas densities are exceptionally large and enormous amounts of energy and angular momentum are released as the material accretes onto the supermassive nuclear engine. Performing studies of the structure, kinematics and excitation of this material is the sole mean available to investigate (super)massive ultracompact objects.

Because of obscuration and crowding, only a few molecular tracers can provide direct information on the innermost regions of active galaxies. The H2O $\lambda=1.3$ cm maser line, profiting from a long wavelength (no obscuration by dust grains), from its enormous luminosity (up to 104 $L{_\odot}$ (isotropically), corresponding to $\sim $1053 photons/s; see Koekemoer et al. 1995; Barvainis & Antonucci 2005) and the availability of Very Long Baseline Interferometry (VLBI) networks, is a particularly suitable tracer of this environment. The line samples gas with kinetic temperatures of several 100 K and densities of $\sim $108 cm-3 (e.g., Kylafis & Norman 1987, 1991).

So-called "disk-masers'' as in NGC 4258 allow us to map nuclear accretion disks (e.g. Greenhill et al. 1995; Miyoshi et al. 1995; Herrnstein et al. 2005). Analysis of the dynamics of observed Keplerian disks leads to estimates of the mass of the nuclear engine and to a determination of the distance to the galaxy, independent of any standard candles. So-called "jet-masers'' as in Mrk 348 (Peck et al. 2003) are associated with the pc-scale jets and provide estimates, through reverberation mapping, of the speed of the material in the jet. A further class of masers is associated with nuclear outflows (Circinus; Greenhill et al. 2003).

Measuring the proper motion of galaxies has been another long-standing problem. The solution is to find sufficiently luminous ultracompact sources that can be observed with VLBI techniques involving phase referencing. Extragalactic H2O masers are suitable targets and could provide, through their measured radial velocities and proper motions, three dimensional velocity vectors in space (Brunthaler et al. 2005, 2007), not only for the masers themselves but also for the nuclei of their parent galaxies.

Based on the assumption that the water masers are located in circumnuclear tori, (often) aligned with the nucleus and amplifying its continuum, linearly for saturated masers and exponentially for unsaturated ones, one should expect a high detection rate in radio-loud galaxies (in particular those with the radio axis close to the plane of the sky). However, water megamasers have been found so far only in low-radio power AGN ( $P_{\rm 1~GHz} < 10^{22-23}~\rm W~Hz^{-1}$), mostly in galaxies classified as Sy 2s or LINERs (Braatz et al. 1996, 1997).

A first systematic search for the $\lambda=1.3$ cm line in radio galaxies was performed by Henkel et al. (1998). No maser was detected in a sample of $\sim $50 Fanaroff-Riley type I (FR I) galaxies. Subsequently, targets belonging to the more powerful Fanaroff-Riley type II (FR II) class were observed by two groups (Tarchi et al., Lara et al., unpublished) again with negative results.

According to the current paradigm for radio-loud AGN, FR II galaxies host type 2 AGN with narrow optical emission lines and prominent, extended nuclear jets. Since the jets are ejected at a small angle with respect to the plane of the sky, FR II galaxies should contain a nuclear torus being viewed approximately edge-on (for a review, see e.g. Urry & Padovani 1995). So far, however, the presence and nature of these hypothesized tori has remained an enigma. The nuclear region of the prototypical FR II galaxy Cyg A shows evidence for dust and obscuration with gas column densities up to several 1023 cm-2. Morphology and physical parameters of the nuclear region as well as the mechanism triggering nuclear activity are, however, not yet fully understood (e.g., Conway & Blanco 1995; Carilli & Barthel 1996; Fuente et al. 2000; Bellamy & Tadhunter 2004).

Very recent modifications to the standard unified scheme (hereafter SUS) state that FR I galaxies (or at least the majority of them) seem to lack a geometrically and optically thick molecular torus. This scenario is now supported by an increasing number of studies (e.g., Chiaberge et al. 1999; Perlman et al. 2001; Verdoes Kleijn et al. 2002; Whysong & Antonucci 2004). In order to account for the absence of broad emission lines in narrow-lined FR IIs (within the framework of the SUS believed to represent the parent population of radio-loud quasars) a geometrically and optically thick obscuring layer is required instead (Barthel 1989, and references therein).

Recently, a luminous ( $L_{\rm H_2O}\sim10^3$ $L{_\odot}$) H2O megamaser has been detected in 3C 403 (Tarchi et al. 2003; hereafter THC), an FR II galaxy at roughly the same distance as Cyg A. 3C 403 is the first and so far only powerful radio galaxy with a detected H2O maser.

The kpc radio morphology of 3C 403 is typical for X-shaped radio galaxies. The cause of the "X'' radio shape is still debated. Arguments exist that support the origin of this peculiar morphology as due to a sudden change in the jet direction. Merritt & Eckers (2002) have argued that the sudden change in the jet direction reflects a sudden (<few yr) change in the black hole spin axis due to a black hole merger (see also Sect. 5.2.2). Alternative models imply instead slow precession of the jet axis or lobe backflow (see Dennett-Thorpe et al. 2002; Schoenmakers et al. 2000).

The Very Large Array (VLA) $\lambda=3.6$ cm maps of Black et al. (1992; hereafter BBL; their Fig. 13) and Dennett-Thorpe et al. (2002; hereafter DSL; their Fig. 1) show two bright radio lobes towards the east and west with hot-spots and two weaker, longer and broader wings to the north-west and south-east. The two bright lobes are caused by jets containing a number of prominent knots. Adopting a WMAP cosmology (H0=71, $\Omega_{\rm M}=0.27$, $\Omega_\lambda=0.73$; Spergel et al. 2003), the redshift of z=0.059 leads to an angular size distance of $D_{\rm A}\sim 230$ Mpc, at which 1 mas corresponds to $\sim $1.1 pc.

In this paper, we present results from a follow-up VLA A-array observation of the maser emission and the outcome of a search for CO emission using the 30-m IRAM telescope at Pico Veleta. We also discuss monitoring observations of the maser line spanning two years. Furthermore, to obtain a more realistic picture of the innermost regions of 3C 403 and to find out whether an accretion disk scenario is plausible, we mapped the 6 cm radio continuum emission with parsec scale resolution using the European VLBI Network (EVN).

  
2 Observations and data reduction

Effelsberg 3C 403 was observed in the 616 - 523 transition of H2O (rest frequency: 22.23508 GHz) with the 100-m telescope of the MPIfR at Effelsberg[*] at four epochs between January 2003 and April 2004. The beam width was 40''. The observations were made with a 18-26 GHz HEMT receiver that was sensitive to the two orthogonal linear polarizations. A dual beam switching mode with a beam throw of 2$^\prime$ and a switching frequency of $\sim $1 Hz was chosen. The Effelsberg AK90 spectrometer was used as backend. System temperatures, including atmospheric contributions, were $\sim $40-60 K on an antenna temperature scale ( $T_{\rm A}^*$). The beam efficiency was $\eta_{\rm b}\sim0.5$. Flux calibration was obtained by measuring W3(OH) (see Mauersberger et al. 1988). Gain variations of the telescope as a function of elevation were taken into account (see e.g., Eq. (1) of Gallimore et al. 2001). The pointing accuracy was better than 10 $^{\prime\prime}$. All data were reduced using standard procedures of the GILDAS software package (http://www.iram.fr/IRAMFR/GILDAS/).

GBT Observations were made with the Green Bank Telescope (GBT) of the NRAO[*] during six sessions between 2003 October 20, and 2005 February 15. We used the 18-22 GHz K-band receiver, which has two beams at a fixed separation of 3$^\prime$ in azimuth. The GBT beamwidth is 35 $^{\prime\prime}$ at the red shifted maser frequency of 21 GHz, and pointing uncertainties were better than 10 $^{\prime\prime}$. The data were taken in total power mode, and the telescope was nodded between two positions on the sky such that the source was always in one of the two beams during integration. We used a nod cycle of 2 min per position.

The spectrometer was configured with two 200 MHz bandpasses, one centered on the systemic velocity of 3C 403 and the second redshifted by 180 MHz. No emission was detected beyond what is shown in Fig. 1. The zenith system temperature was between 35 and 45 K. Atmospheric opacity was estimated using system temperature and weather data, and ranged from 0.04 to 0.06 at the zenith. We reduced the data using GBTIDL.


  \begin{figure} \par\includegraphics[width=7.4cm,clip]{8317f1.eps}\end{figure} Figure 1: Maser lines in 3C 403 observed with Effelsberg (four epochs), the GBT (6 epochs), and the VLA (one epoch). The spectrum from the first epoch (upper panel) was already published in THC. The channel spacing is 312 kHz ($\cor$4.5 km s-1), 195 kHz ($\cor$2.8 km s-1), and 391 kHz ($\cor$5.6 km s-1) for the spectra taken with Effelsberg, the GBT, and the VLA, respectively. Zero velocity corresponds to a frequency of 20996.28 MHz (c z = 17 688 km s-1 w.r.t. the Local Standard of Rest (LSR)), the galaxy's recessional velocity according to the NASA/IPAC database (NED).
Open with DEXTER

VLA Water maser emission was observed at the red shifted maser frequency of 21 GHz on July 23 and 25, 2003, with the Very Large Array (VLA) of the NRAO2 in its A configuration for an 8 h total on-source time. We observed with two 12.5 MHz IFs centered on the two maser features detected by Tarchi et al. (2003; see the upper spectrum of Fig. 1). Each IF was split into 32 channels providing a channel spacing of $\sim $6 km s-1. The source 1331+305 (2.66 Jy) was used as flux and bandpass calibrator. The point source 1950+081, at a distance of 5 $.\!\!^\circ$6 from 3C 403 (there was no suitable closer source), was used for phase calibration. The two IFs were calibrated separately and then combined (AIPS task: UVGLU) yielding a total velocity coverage of $\sim $360 km s-1. The data were Fourier-transformed using natural weighting to create a $256\times256\times64$ data cube. The radio continuum was subtracted using the AIPS task UVLSF. This task fits a straight line to the real and imaginary parts of selected channels and subtracts the fitted baseline from the spectrum, optionally flagging data having excess residuals. In addition, it provides the continuum as a UV data set, which has been used to create continuum maps of the galaxy. The restoring beam is $0~\hbox{$.\!\!^{\prime\prime}$ }1\times0~\hbox{$.\!\!^{\prime\prime}$ }1$. The rms noise per channel becomes 0.6 mJy, consistent with the expected thermal noise.

EVN 3C 403 was observed on May 20, 2004, with the European VLBI Network[*] (EVN) at 6 cm. Eight 8 MHz bands, each at right and left circular polarization, were employed. The total observing time was 10.5 h. We used 4C +02.49 as a phase-reference source and switched every 2 min between the two sources. The initial calibration was performed with the AIPS package. A priori amplitude calibration was applied using system temperature measurements and standard gain curves. Fringes were found in the 3C 403 data itself on all baselines, so we used this source as phase-reference and applied the solutions also to 4C +02.49. The data were self-calibrated and mapped using the software package DIFMAP (Shepherd et al. 1994). We started with phase-only self-calibration and later included phase-amplitude self-calibration with solution intervals slowly decreasing down to one minute.

Pico Veleta 3C 403 was observed in a search for CO emission on November 6, 2004, using the IRAM[*] 30-m telescope at Pico Veleta, Spain. Using the A/B receiver combination we searched simultaneously for CO(1-0) and CO(2-1) with the A/B 100 receivers tuned to 108.85 GHz and the A/B 230 receivers tuned to 217.69 GHz. Beamwidths were 23 $^{\prime\prime}$ and 13 $^{\prime\prime}$, respectively. Spectra were obtained using the wobbler switch technique with a beam throw of 60 $^{\prime\prime}$ and a switching frequency of 0.5 Hz. The data were recorded using the 1 MHz (512 channels, 1 MHz channel spacing) and 4 MHz (256 channels, 4 MHz channel spacing) filterbanks for the 109 and 218 GHz observations, respectively. The effective velocity coverage is 1400 km s-1 at both frequencies. Typical system temperatures were 160 and 500 K ( $T_{\rm A}^*$). The fast switching procedure and the good quality of the resulting baselines also provide a rough measure of continuum levels (see Sect. 4.1.3). 3C 403 was observed for about 70 min (on+off) leading to rms noise levels of 4.2 and 12.5 mJy after smoothing the 109 and 218 GHz spectral bands to channel widths of 44 and 50 km s-1.

  
3 The systemic velocity of 3C 403

For the following sections it is of fundamental relevance to assess the accuracy of the reported systemic velocity $V_{\rm sys}$ of 3C 403. Optical emission line measurements indicate $V_{\rm sys} = 17~688$ km s-1 (z = 0.059) with no uncertainty value provided (Spinrad et al. 1985, and references therein). Previous studies indicate that recessional velocities of galaxies derived from optical emission lines tend to have a systematic uncertainty, often being smaller than systemic velocities derived from H I (e.g. Mirabel & Wilson 1984; Morganti et al. 2001). This difference is attributed to a net outflow of gas in the optically unobscured front side of narrow emission line regions (e.g. Mirabel & Wilson 1984). Unfortunately, no neutral hydrogen has been so far detected in 3C 403 (see Sect. 5.1.2) to perform a comparison with the optically-derived recessional velocity. Baum et al. (1990), while not providing a recessional velocity, derived on the basis of [O I], [N II], H$\alpha$ and [S II] data a rotation curve of 3C 403 that indicates no strong anomalies. From this we conclude that the uncertainty in $V_{\rm sys}$, as derived by Spinrad et al. 1985, should not exceed 100 km s-1.

4 Results

4.1 Spectral line emission

4.1.1 Maser monitoring

Figure 1 shows the water maser spectra from 3C 403 at eleven epochs from January 2003 to February 2005, observed with the Effelsberg telescope, the GBT, and the VLA A-array. Past Effelsberg unpublished data from December 1997 showed no sign of emission at a 3$\sigma$ level of 60 mJy. Figure 2 displays our most sensitive spectrum, that obtained with the VLA indicating the possible presence of three features that, for the sake of convenience, we indicate as component I, II, and III.


  \begin{figure} \par\includegraphics[width=7.3cm,clip]{8317f2.eps}\end{figure} Figure 2: The main water maser features in 3C 403 observed with the VLA A-array on July 23, 2003 (see Sect. 4.1.2 and Fig. 1). The dashed vertical line marks the nominal systemic velocity of the galaxy, $V_{\rm sys}$ = c z = 17 688 km s-1.
Open with DEXTER

The most obvious change that can be deduced from Fig. 1 is that, in the early spectra, emission is mostly present on the red-shifted side (component I), while later most of the emission (component II) is blue-shifted w.r.t. the systemic velocity. In January and March 2003, component I had a peak line strength of 20-25 mJy, becoming weaker at subsequent epochs and remaining undetected in the most recent spectra (<5 mJy). Component II correspondingly increases its flux from $\sim $4 to 20 mJy before significantly fading in the last two spectra. From March 2003 to January 2004, component II seems to experience a first shift from about -45 to -95 km s-1 and a second one back to about -60 km s-1 in February 2005. Of course, the possibility that there is actually no shift and we are, instead, witnessing the brightening and fading of different components is also a possibility. Component III, detected at a low significant level only in the first three spectra, fades below the 5 mJy noise level together with component I.

While no systematic regular velocity drift involving all the feature can be confidently observed, it is remarkable that within about 15 months the maser lines swapped their intensities. A time scale of one year and peak flux densities of order 20 mJy indicate an angular source size of $\la$0.3 mas and a peak brightness temperature of $\ga$5$\times $108 K, if variations are intrinsic to the cloud(s) and are not triggered by fluctuations of the continuum background. Each individual component reaches peak isotropic luminosities well in excess of 1000 $L{_\odot}$. So far, only four other maser sources were reported to have a similar power, TXS22226-184 (Koekemoer et al. 1995), Mrk 034 (Henkel et al. 2005), J0804+3607 (Barvainis & Antonucci 2005), and UGC 5101 (Zhang et al. 2006). A variation by more than a factor of two has not yet been reported in such a luminous maser component. Less luminous masers with linewidths in excess of 10 km s-1 are commonly more stable.


  \begin{figure} \par\includegraphics[width=6.8cm,clip]{8317f3.eps}\end{figure} Figure 3: Close-up of the region around the nucleus of 3C 403. Shown as a filled triangle, a cross, and a filled square are the variance-weighted average locations with error bars of maser components I, II, and III, respectively. Position offsets in (RA $_{\rm J2000}$, Dec $_{\rm J2000}$) are relative to the 22-GHz continuum peak position.
Open with DEXTER

  
4.1.2 The VLA view of the H2O maser

In all VLA velocity channels (see Fig. 2; for a preliminary report, see also Tarchi et al. 2005) the emission peaks at the position RA $_{\rm J2000}$ = 19$^{\rm h}$ 52$^{\rm m}$ 15 $.\!\!^{\rm s}$80, Dec $_{\rm J2000}$ = 02 $^{\rm\circ}$ 30 $^{\rm\prime}$ 24 $.\!\!^{\prime\prime}$2. The nominally estimated error for absolute positions for a VLA A-array map is 0  $.\!\!^{\prime\prime}$1 when a strong nearby calibrator can be used for phase referencing (as done in our observations, using the source 1950+081). Since we have also used the "fast switching'' technique, this error can be taken as a safe upper limit.

The total integrated intensity (moment-0; in mJy km s-1 beam-1) VLA plots of components I-III show that they are unresolved at the 0  $.\!\!^{\prime\prime}$1 resolution and coincident in position with the radio continuum nucleus of the galaxy (see also Sect. 4.2.1). The alignment between line and continuum peak positions derived from the same data is only limited by the signal-to-noise ratios (SNRs) and is estimated to be $\sigma_{\rm rel} = \sqrt{(\theta_{l}/2 \cdot {\it SNR}_{l})^{2} + (\theta_{\rm... ...t {\it SNR}_{\rm c})^{2}} = \sqrt{(0.1/2 \cdot 15)^{2} + (0.1/2 \cdot 160)^{2}}$ $\sim $ 0 $.\!\!^{\prime\prime}$005 $\cor$ 5.5 pc, where $\theta$ denotes the restored beam size, and l and c refer to line and continuum emission, respectively.

Figure 3 presents a close-up of the region around the nucleus of 3C 403, showing the relative distribution of maser components I, II, and III. The symbols and error bars mark the variance-weighted average locations and uncertainties of the three maser components derived fitting, with the AIPS task JMFIT[*], the maser emission in each channel with flux density >5 times the rms noise of 0.6 mJy beam-1. Our result indicates an upper limit for the offset between different components of $12 \pm 4.5$ mas. The red-shifted emission (components I and II) is seemingly located eastwards w.r.t. the blue-shifted one (component II).

In addition, we have produced a $\sim $ $3^{\prime}\times3^{\prime}$ map, covering the entire radio extent of the galaxy and no additional maser spots were detected above the 0.6 mJy level given in Sect. 2.


  \begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{8317f4.eps}\end{figure} Figure 4: 30-m IRAM telescope CO(1-0) (solid lines) and CO(2-1) (dotted lines) spectra of 3C 403. The data were smoothed to channel widths of 44 and 50 km s-1, respectively. The zero velocity corresponds to the recessional velocity of the galaxy ( $V_{\rm sys}$ = 17 688 km s-1).
Open with DEXTER

  
4.1.3 CO spectra and millimeter wave continuum

Motivated by the detection of megamaser emission, we searched for the two ground rotational transitions of the most common observable molecule, CO. Unlike 22 GHz H2O, the CO (1-0) and (2-1) lines predominantly trace cool, low-density gas. No clear emission is seen down to 3$\sigma$ noise limits of 13 and 38 mJy for the two respective transitions (this refers to the unsmoothed spectra with 1 and 4 MHz channel spacing, see Sect. 2). We tentatively detect emission at $\sim $-300 km s-1 with respect to the systemic velocity (Sect. 3). Evans et al. (2005) also reported a non-detection of CO toward 3C 403 as part of a survey of IRAS radio galaxies. Curiously, also in their spectrum (their Fig. 1) a highly tentative feature is present at about -300 km s-1. While the offset is opposite to that expected from optical emission lines (Sect. 3) and while evidence for such a feature is too weak to seriously question the recessional velocity adopted throughout this paper, a CO spectrum with higher sensitivity would be desirable.

Indicated by the baselines, continuum emission was also detected. At 109 GHz, the level is approximately $25 \pm 13$ mJy (the uncertainty was estimated from the variations of the continuum level in individual scans). No continuum was detected at 218 GHz.


  \begin{figure} \par\includegraphics[width=7.21cm,clip]{8317f5.ps}\end{figure} Figure 5: A naturally weighted 22 GHz VLA radio continuum image (resolution: 0  $.\!\!^{\prime\prime}$1, corresponding to $\sim $115 pc) of the nuclear region of 3C 403, made using channels free of line emission. The peak is at 40 mJy beam-1. The contours are (-1, 1, 2, 4, ..., 32) $\times $ 0.75 mJy beam-1.
Open with DEXTER

4.2 Continuum emission

  
4.2.1 22 GHz VLA emission

In Fig. 5, we present a naturally weighted VLA A-array 22 GHz radio continuum image of the nuclear region of 3C 403, produced using maser emission-free channels. The source is spatially unresolved with a peak flux density of 40 mJy beam-1. However, an elongation is apparent in the uniformly weighted image of Fig. 6 that might be a weak signature of a parsec scale jet visible in the higher resolution images presented in Sect. 4.2.2.

As for the H2O line emission, we have also investigated a $\sim $ $3^{\prime}\times3^{\prime}$ area in a search for additional radio continuum emission. Apart from the nucleus, among the radio continuum features (lobes, radio jets, and bright knots) reported by BBL and DSL, we have only detected emission at position RA ${\rm _{J2000}} = 19^{\rm h} 52^{\rm m} 17.6^{\rm s}$, Dec ${\rm _{J2000}}= 02^{\rm\circ} 30^{\rm\prime}33^{\rm\prime\prime}$, coincident within the errors with the exceptionally bright radio knot F6 (nomenclature according to BBL). The knot in our map (Fig. 7) seems to be resolved into two components aligned almost perpendicular to the large scale radio jet. Using a 500 k$\lambda $ taper function, weak emission is also detected at the position where two compact structures in the eastern hotspot (F1 and F2, following BBL) have been previously observed (Fig. 8). The remaining radio emission from 3C 403 detected by DSL is either resolved out or is below the detection threshold given in Sect. 2.


  \begin{figure} \par\includegraphics[width=7.21cm,clip]{8317f6.ps}\end{figure} Figure 6: A uniformly weighted 22 GHz VLA radio continuum image (resolution: 0  $.\!\!^{\prime\prime}$08, corresponding to $\sim $90 pc) of the nuclear region of 3C 403, made using channels free of line emission. The peak is at 39 mJy beam-1. Contours are (-1, 1, 2, 4, ..., 32) $\times $ 0.75 mJy beam-1.
Open with DEXTER


  \begin{figure} \par\includegraphics[width=7.21cm,clip]{8317f7.ps}\end{figure} Figure 7: A naturally weighted 22 GHz VLA radio continuum image (resolution: 0  $.\!\!^{\prime\prime}$1, corresponding to $\sim $115 pc) of the bright radio knot (F6, following DSL) in 3C 403, obtained from channels free of line emission. The peak is at 1.5 mJy beam-1. Contours are (-1, 1, 1.5, 2) $\times $ 0.6 mJy beam-1.
Open with DEXTER


  \begin{figure} \par\includegraphics[width=7.1cm,clip]{8317f8.ps} % \end{figure} Figure 8: A 500 k$\lambda $ tapered 22 GHz VLA radio continuum image (resolution: 0  $.\!\!^{\prime\prime}$33, corresponding to $\sim $375 pc) of the compact hotspot structures (F1 and F2, following BBL) in 3C 403, made using channels free of line emission. The peak is at 2.5 mJy beam-1. The contours are (-1, 1, 1.5, 2, 2.5) $\times $ 0.9 mJy beam-1.
Open with DEXTER

  
4.2.2 VLBI maps

Milliarcsecond resolution 6-cm VLBI maps of the radio nucleus of 3C 403 are shown in Figs. 9 and 10. The visibilities of 3C 403 demonstrate that the source is resolved at longer baselines (Fig. 11). The amplitude drops from 70 mJy at the shortest baselines (10 M$\lambda $) to 40 mJy at 60 M$\lambda $.


  \begin{figure} \par\includegraphics[width=8.3cm,clip]{8317f9.eps}\end{figure} Figure 9: Full resolution EVN image of the nucleus of 3C 403 at $\lambda =6$ cm. The contours start at 0.2 mJy and increase with a factor of 1.5. The beam size of the observations is 1.87 mas $\times $ 0.94 mas at a position angle of 76 $~.\!\!^{\circ}$9.
Open with DEXTER


  \begin{figure} \includegraphics[angle=-90,width=8.3cm,clip]{8317f10.ps}\end{figure} Figure 10: Low resolution EVN image of the nucleus of 3C 403 at $\lambda =6$ cm using only the continental EVN antennas. The contours start at 0.35 mJy and increase with a factor of 1.5. The beam size is 6.05 mas $\times $ 4.67 mas at a position angle of 67 $~.\!\!^{\circ}$4.
Open with DEXTER


  \begin{figure} \includegraphics[angle=-90,width=8.3cm,clip]{8317f11.ps}\end{figure} Figure 11: The visibilities of 3C 403 clearly show that the source is resolved on the longer baselines.
Open with DEXTER

The uniformly weighted VLBI map of 3C 403 is shown in Fig. 9. Notable are extensions to the north-east and south-west. We fitted circular Gaussian components to the uv-data, and the best fit with three components gave a reduced $\chi^2$ per degree of freedom of $\sim $1.7. Reducing the number of components to two or one increases the reduced $\chi^2$ p.d.f. to 2.2 and 2.9, respectively. On the other hand, adding more components does not significantly improve the fit. Hence, we used a three component model and the results from this fit are shown in Table 1. We fitted the three components many times with different initial parameters and used the scatter in the results to estimate the uncertainties of the fit parameters. While the flux densities and angular sizes of the three components are not strongly constrained by the fit, the position angle is well determined. The orientation of the pc-scale jet is in very good agreement with the kpc-scale jet seen on VLA images.

Since the telescope in Urumqi (China) could not take part in the observations, all information on the long baselines is based on only two telescopes, Hartebeesthoek (South Africa) and Shanghai (China). Hence the data on long baselines, mainly responsible for the uncertainties in the model fit parameters in Table 1, should be considered with some caution. To test the result shown in Fig. 9 we also self-calibrated and imaged the data from the short baselines only. As before, the amplitude in the visibilities shows a slow decrease towards longer baselines. The resulting map is shown in Fig. 10. The extension toward the north-east is visible in this map and there might be also a weak jet component towards the south-west. From this we conclude that the weak extensions on mas scales are real and are not caused by amplitude calibration errors.

Table 1: Model fit of the three components A, B, and C to the uv-data. S is the flux density, d denotes the separation from the phase center.

Assuming the presence of a core and one or two nuclear jet components, there are three interpretations:

5 Discussion

  
5.1 Evidence for an edge-on torus

5.1.1 The radio continuum

To select the most likely of the three scenarios outlined in Sect. 4.2.2 and to identify the location of the radio nucleus, we compare our continuum VLBI maps with the large scale structure of 3C 403. The orientation of component A ( $\rm PA=73^\circ$; Table 1) is in very good agreement with the eastern large scale jet and the position of a bright knot (73$^\circ$) in its lobe (e.g., BBL, DSL). The south-western jet (component C), as seen in Fig. 9, seems to bend slightly to the west, thus pointing towards the western large scale jet. In view of the limited uv-coverage w.r.t. long baselines (see Sect. 4.2.2), we consider this latter coincidence as tentative.

The presence of the western and eastern large scale jets with similar flux densities suggests that the jets must lie close to the plane of the sky. The inner 10 pc of 3C 403 (Figs. 9 and 10) show a similar morphology. Thus a scenario with B representing the core and A and C marking jet and counterjet is by far the most likely one. If we see the jet and the counterjet with similar strengths, the orientation of the jets must be close to the plane of the sky. This view is supported by Kraft et al. (2005; hereafter K05). They present results from Chandra X-ray observations and describe the X-ray spectrum of the nucleus as a superposition of two power-law continuum components with a 6.4 keV Fe line. One of these power-law components is heavily absorbing ( $N_{\rm H}\sim 4\times10^{23}$ cm-2).

If the X-ray photons are predominantly scattered radiation not passing through the main body of the obscuring torus, the high column density derived by K05 would only be a lower limit. Since no evidence was found for a significant amount of dust in observations with the Hubble Space Telescope (Martel et al. 1999), K05 conclude that the absorption is due to material close to the nuclear engine, possibly forming a molecular torus. Spectroscopic studies at optical wavelengths revealed narrow emission lines (Tadhunter et al. 1993), indicating that the broad line region is hidden behind an edge-on dusty torus.

5.1.2 On the absence of HI and CO

Morganti et al. (2001) searched for H I absorption in 3C 403 and got an upper limit of $N_{\rm H} < 5 \times 10 ^{20}$ cm-2 ( $T_{\rm spin} = 100$ K). Large differences in H I and X-ray column densities are quite common in Seyfert galaxies (e.g. Gallimore et al. 1999). The striking discrepancy between X-ray (Sect. 5.1.1) and H I column densities indicates the predominance of either ionized or molecular gas along the line of sight toward the nuclear source of 3C 403. While both kinds of environment may coexist in a small volume surrounding the central engine, the maser emission provides substantial evidence for the latter.

Why are we then not seeing CO? For a quasi-thermally excited line, seen in emission, beam dilution may become important in an object as distant as 3C 403. With the observed brightness temperature as a function of the intrinsic one as well as source and beam solid angle ( $T_{\rm b}^{\rm obs}$ = [ $T_{\rm b}^{\rm int}$ $\times $ $\Omega_{\rm torus}$]/[ $\Omega_{\rm torus}$ + $\Omega_{\rm beam}$]) we can determine the smallest toroid size, $\Omega_{\rm torus}$, we would have detected. With a CO line detection threshold of $T_{\rm mb}^{\rm obs}$ = 1.8 mK and a 109 GHz beam size of 23 $^{\prime\prime}$ (Sect. 2), we obtain $\Omega_{\rm torus}$ $\sim $ 0 $~.\!\!^{\prime\prime}$04 $\times $ (500 K/ $T_{\rm b}^{\rm int}$)1/2 that corresponds to a linear scale of $\sim $ 50 pc $\times $ (500 K/ $T_{\rm b}^{\rm int}$)1/2. Elliptical galaxies are characterized by high stellar velocity dispersions efficiently heating any cool gas and creating an X-ray emitting plasma that is greatly confining the volume occupied by molecular clouds (e.g., Wiklind & Henkel 2001). The lack of dust emission (Martel et al. 1999) supports a small size of the molecular complex in the nuclear region and is therefore consistent with our non-detection of CO.

For the absence of deep CO J = 1-0 absorption against the nuclear radio continuum source (the absorption must reach a significant fraction of the continuum level, otherwise it would not be detected; see Sect. 4.1.3 and Fig. 4), there are several possible explanations. (1) There is no molecular gas in front of the nuclear source. In view of the column density (K05) this is not likely. (2) The torus is partly or entirely molecular but has a very small fractional CO column density in the J = 0 and 1 states. This may be a consequence of a high temperature of the gas, possibly coupled with an intense radiation field (resulting in excitation temperatures of several 100 to $\sim $2000 K). (3) The obscuring clouds may be much smaller than the radio continuum source, similar to what was proposed for the much stronger radio emitter Cyg A by Barvainis & Antonucci (1994). Within this context the size of the H2O maser hotspots (Sect. 4.1.1) does not provide any guideline, because 22 GHz H2O emission may originate from much higher density gas then the ground rotational lines of CO. (4) Alternatively, it is also possible that any existing absorption would be "swamped'' by emission at the same velocity interval.

5.2 Origin of the H 2O maser emission

5.2.1 Constraints on the application of the standard model

The main result of our VLA observations is that the two 22 GHz H2O velocity components of 3C 403 do not arise from the extended lobes of the system, but are aligned with the central radio continuum source within a $\sim $5.5 pc sized region. Furthermore, the nuclear torus likely has an edge-on orientation (see Sect. 5.1). Thus an association of the maser features with a dense circumnuclear torus/accretion disk is a possibility worth discussing.

To analyze this case, we have to evaluate the statistical properties of the sample of known megamaser galaxies. Accounting for the sources given in Henkel et al. (2005), Kondratko et al. (2006), and Zhang et al. (2006), the latter containing 64 galaxies with detected H2O emission beyond the Magellanic Clouds, there are a total of 51 known megamaser sources ( $L_{\rm H_2O}> 10$ $L{_\odot}$). Most of these have not yet been studied in spatial detail. Omitting 3C 403, the sample contains two pure jet-masers (apparent interaction between a nuclear jet and a dense molecular cloud), while 16 sources appear to be disk-masers arising from an accretion disk. The latter is either based on detailed observations as in the case of NGC 4258 (e.g., Miyoshi et al. 1995) or, a little more speculative, on the measured lineshape (see, e.g., NGC 6323 in Braatz et al. 2004). H2O megamaser emission associated with a nuclear outflow is only known for one source of the sample, the Circinus galaxy. Even here, however, only a part of the emission is associated with the outflow, complementing a nuclear accretion disk viewed approximately edge-on (Greenhill et al. 2003).

In view of the known sample of megamaser galaxies, an association of the maser in 3C 403 with a nuclear outflow appears to be unlikely. So far all detected "jet-maser'' components are observed at one side w.r.t. the systemic velocity (Henkel et al. 2005). We should keep in mind, however, that 3C 403 is an (elliptical) FR II and not a (spiral) Seyfert 2 or LINER galaxy and that "disk-masers'' may be identified more easily than "jet-masers''. Nevertheless, observed lineshapes and the relatively large number of disk masers superficially hint toward H2O emission from an accretion disk as the most plausible interpretation of the H2O lines from 3C 403.

If the emission were part of an accretion disk, at which galactocentric radius would it arise? Assuming that the two spectral components originate from the tangentially seen parts of a nuclear accretion disk seen approximately edge-on ($i \sim 90$ $\hbox{$^\circ$ }$), we obtain (Fig. 1) a rotation velocity of $V_{\rm rot} = V_{\rm obs}~\sin^{-1} i$ $\sim $100 km s-1. From Bettoni et al. (2003; their Table 3) we obtain $M_{\rm BH} = 10^{8.8}$ $M_{\odot}$ as the mass of the nuclear engine. Combining these two parameters and assuming the presence of Keplerian rotation (as in NGC 4258, see Miyoshi et al. 1995; Herrnstein et al. 1999, 2005), this yields with

\begin{displaymath}R = 0.89 \left[\frac{M_{\rm BH}}{M_{\odot}}\right] \left[\fr... ...}}\right]^{-2} \left[\frac{D}{\rm Mpc}\right]^{-1} {\rm mas} \end{displaymath}

an angular distance of 245 mas, corresponding to a galactocentric radius of $R_{\rm GC}$ $\sim $ 275 pc. This size conflicts with the result of our VLA observations (Sect. 4.1.2) that, indicating that the continuum and the H2O emission are arising from the same 5.5 pc (5 mas) sized region, imply a maximal galactocentric radius for the H2O masers of 2.75 pc (2.5 mas).

Is it possible to reconcile this value with the possibility that the maser arises in an accretion disk like that in NGC 4258? A 2.75-pc radius disk rotating at 100 km s-1 would imply a black hole mass $M_{\rm BH}$ = 106.8 $M_{\odot}$, a factor of 100 lower than that derived by Bettoni et al. 2003. Alternatively, we might consider a disk inclined by $\sim $6 $\hbox{$^\circ$ }$ or less. However, this would describe an almost face-on disk, a scenario not only different from that of NGC 4258 but also seemingly contradicting the presence of jets oriented approximately along the plane of the sky.

To summarize, the masers in 3C 403 are peculiar in three different ways. (1) They are detected at the core of a radio galaxy. (2) The two main ultraluminous velocity components are highly time variable and (3) the Keplerian model seems to fail. If the main velocity components do not represent the two tangentially viewed parts of the masing disk but instead only one part and the systemic features, this would lead to $V_{\rm rot}\sim200$ km s-1 and with $M_{\rm BH} = 10^{8.8}$ $M_{\odot}$ (Bettoni et al. 2003) to a galactocentric distance of 60 mas (70 pc). In this case the disagreement with observations is slightly less severe but the linear scale is still inconsistent with the results from our VLA A-array measurements (Sect. 4.1.2). Thus, the accretion disk scenario requires relatively strict constraints to be applied to our case unless we are only viewing the systemic velocity features of the putative maser disk (see below).

5.2.2 Alternatives to the accretion disk scenario

Cloud stability considerations: A main difference between Seyfert and FR II galaxies (equivalent to radio loud type 2 quasars according to the standard unified scheme) is the mass of the nuclear engine. While in Seyfert galaxies masses range from $\sim $106 to a few 107 $M_{\odot}$ (e.g., Greenhill et al. 1996, 1997; Herrnstein et al. 1999; Henkel et al. 2002), masses in radio galaxies and quasars reach 109 $M_{\odot}$, with 3C 403 hosting a nucleus that is not far below this latter value (Bettoni et al. 2003). Could clouds in an NGC 4258-like disk that is characterized by a particularly large rotational velocity and small galactocentric radius be stable in an environment dominated by such a large central mass?

The masers in NGC 4258 might arise from well confined discrete clumps that are encompassing only a small fraction of the entire volume of the warped circumnuclear disk. For a roughly spherical clump at distance $R_{\rm GC}$ from the central engine and neglecting magnetic fields (see Modjaz et al. 2005), a density of

\begin{displaymath}n({\rm H_2}) \ga\ \frac{3}{2~\pi~{\rm G}} \ \left( \frac{V_{\rm rot}}{R_{\rm GC}} \right)^2 \end{displaymath}

is required to reach stability against tidal disruption (Stark et al. 1989). G is the gravitational constant. For NGC 4258, i.e. $R_{\rm GC} \sim 0.2$ pc and $V_{\rm rot} \sim 1000$ km s-1 (Herrnstein et al. 1999, 2005), the resulting density becomes n(H2) $\sim $ $5\times10^{10}$ cm-3. This is close to thermalization (Kylafis et al. 1991). For commonly accepted collisional excitation this either hints at excitation by a two temperature gas (e.g., Kylafis et al. 1987) or at emission from turbulent, warm, dense molecular debris that does not form self-gravitating clouds.

Most circumnuclear maser disks are characterized by smaller rotation velocities and higher galactocentric distances, significantly reducing the required density for stability against tidal disruption so that here the assumption of long lived masing clumps giving rise to collisionally excited masers is less of a problem (e.g., n(H2) $\ga$ 108 cm-3 in NGC 1068; see Greenhill et al. 1996; Gallimore et al. 2001). Assuming for a putative accretion disk in 3C 403, where only the systemic spectral features are seen (Sect. 5.2.1), $R_{\rm GC}$ = 0.2 pc (as in NGC 4258), the corresponding minimum density for cloud stability reaches, however, 1012 cm-3, which is prohibitively large for collisionally excitated maser emission by a one temperature gas. Could then a lack of stable, well ordered clouds explain the rapid variability of the maser features in 3C 403? At the maximal galactocentric distance permitted by our VLA data, $R_{\rm GC}$ $\sim $ 2.75 pc (Sect. 4.1.2), the required density would drop to more reasonable $\ga$108 cm-3.

The jet-maser scenario: while in Seyfert and LINER galaxies statistics favor accretion disk over jet-masers (Sect. 5.1.1), the two main H2O velocity components are (1) quite broad and (2) offset by several 10 km s-1 from the nominal (NED) systemic velocity of the galaxy. These are the typical spectral properties of jet masers (Peck et al. 2003; Henkel et al. 2005). The flares of velocity components I and II (Fig. 2) may arise from shocked regions at the interface between the energetic jet material and the molecular gas of the cloud the jet is boring through. The time delay between components I and II (Fig. 1) and the apparent red- (component I) and blue-shift (component II) with respect to the systemic velocity may be caused by two clouds at opposite sides of the nucleus that have a slightly different galactocentric radius, possibly being part of a circumnuclear molecular ring.

A binary supermassive black hole in 3C403? Aside from the mass of the nuclear engine, there may be another fundamental difference between 3C 403 and NGC 4258 that is worth mentioning. On a large spatial scale, 3C 403 shows not the standard two-sided radio jet, but a pair of such jets (see Sect. 1). The apparently younger one is oriented roughly NE-SW, the more extended, weaker one in the SE-NW direction. It is thus one of the rare examples of an X-shaped radio galaxy (e.g., Figs. 1 and 2 of Kraft et al. 2005). This morphology is believed to be caused by the coalescence of two supermassive black holes (e.g., Gopal-Krishna et al. 2003; Liu 2004) whose interaction modifies the inclination of the pre-existing nuclear disk of the dominant galaxy. Such a scenario may lead to a complexity that is much higher than that encountered in the nuclear environment of NGC 4258, yielding a puzzling number of possible disk- and jet-maser configurations that have to be constrained by future measurements. In view of the number of free parameters in such an environment, it remains to be seen whether the anticorrelation of the main two maser features was a rare accidental event or whether it will provide an important clue for a better understanding of the so far poorly explored circumnuclear regions of X-shaped radio galaxies.

6 Conclusions and outlook

We have investigated the luminous megamaser in the X-shaped FR II galaxy 3C 403 using single-dish monitoring of the line features and VLA A-array observations. The two main maser features show extreme intensity variations during a two-year period. The position of the maser as derived from the VLA maps is consistent with a location within a few pc of the radio nucleus of the galaxy.

In addition, we have used the EVN to study the galaxy's nuclear radio continuum on parsec scales. A dominant central component and two extensions toward the south-west and north-east are identified. Because these parsec-scale extensions show position angles that are compatible with those of the large scale jets and because these large scale jets show similar flux densities, an interpretation in terms of a dominant nuclear core and a two-sided jet is plausible.

No clear sign of CO emission or absorption has been detected. If emission and absorption are not accidentally canceling each other, this limits the extent of a low density molecular gas component to a size of order $\la$200 pc.

If the mass of the nuclear engine is as large as previously estimated and if the nuclear accretion disk is oriented (as expected) almost edge-on, an NGC 4258-like accretion disk scenario is only viable, if all the detected H2O features are systemic, arising from the front or back side of the disk. There is, however, no observational evidence for the tangentially viewed approaching and receding parts of the disk. A secular velocity drift of the observed components is also not seen. In view of linewidths and deviations from the systemic velocity, an interpretation in terms of "jet-masers'', arising from molecular clouds shocked by the nuclear jet(s), is the most plausible one.

Since 3C 403 is an X-shaped radio galaxy, it may host a binary nuclear engine, greatly enlarging the number of potential scenarios that should be observationally constrained by future measurements. These imply single-dish maser monitoring over long time spans (1) to study the lifetime of the various components, (2) to check whether the anticorrelation of the two main features is a typical or an accidental event and (3) to find, possibly, some evidence for a systematic velocity drift. The latter would be a clear sign for the presence of a nuclear disk even if the red- and blue-shifted parts of this disk remain undetectable (see Wilson et al. 1995, and Braatz et al. 2003, for such a previously identified case). Another very important measurement would be the simultaneous observation of the maser features and the radio continuum at (sub-)milliarcsecond resolution. This could directly show whether the maser features are associated with the nuclear jets or whether we should reject this scenario. In any case it would shed light onto the morphology of the nuclear environment of a prototypical X-shaped galaxy. Finally, systematic monitoring of the radio continuum, H2O and X-ray spectra may provide through reverberation mapping important correlations that would be essential to assess the physical state and three-dimensional morphology of the circumnuclear medium surrounding a 108.8 $M_{\odot}$ AGN.

Acknowledgements
A.T. would like to thank Karl Heinz Wissmann and his collaborators for pleasant discussions during the making of this work. A.B. is supported by the Priority Programme 1177 of the Deutsche Forschungsgemeinschaft. We wish to thank J. Moran for critical comments. This work has benefited from research funding from the European Community's sixth Framework Programme under RadioNet R113CT 2003 5058187. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We have also made use of NASA's Astrophysics Data System.

   
Appendix: 4C +02.49

In order to find suitable phase calibrators for VLBI observations, we observed nine bright and compact sources from the NRAO VLA Sky Survey (NVSS) with an angular separation of <2$^\circ$ with respect to 3C 403. The 22 GHz ( $\lambda \sim1.3$ cm) observations were carried out with the VLA on February 5, 2004. The total observing time was 1.5 h yielding $\sim $4 min on-source integration time per source. The data reduction was performed using standard procedures in the Astronomical Image Processing System (AIPS). The most suitable source w.r.t. morphology and flux density turned out to be 4C+02.49 (see Sect. 2).

The VLA 1.3 cm observations show that 4C+02.49 is a compact double with flux densities of $21.7\pm0.5$ and $15.3\pm0.5$ mJy for the north-eastern and south-western component, respectively (Fig. 12). A broad band radio spectrum of 4C+02.49 (see the inset in Fig. 12) with total integrated flux densities obtained from the NASA Extragalactic Database (NED) and our VLA observation gives a steep spectrum with spectral index of - $1.07\pm0.03$. Hence, this source should be classified as a compact steep spectrum (CSS) source (Fanti et al. 2001). The tight correlation between all data points indicates that there is little variability in the total flux. According to the turnover-frequency vs. linear size relation in CSS sources (O'Dea & Baum 1997), one expects a source size of >10 kpc for a turnover frequency <100 MHz. This cannot be tested, since, so far, no redshift has been derived for this source.


  \begin{figure} \par\includegraphics[width=8cm,clip]{8317f12.eps}\end{figure} Figure 12: VLA map at 1.3 cm ( center) and EVN images ( upper left and lower right) of the two components of 4C +02.49. Also shown is a broad band radio spectrum (upper right) obtained from NED and our VLA 22 GHz flux. The large (blue) crosses indicate flux density measurements that had no error bar.
Open with DEXTER

The two compact components of 4C+02.49 were clearly detected with the EVN at $\lambda \sim6$ cm (Fig. 12). The flux densities are $18.4\pm0.6$ (upper left) and $8.8\pm0.6$ mJy (lower right). Hence, most of the emission that is responsible for the total integrated (NED) 6 cm flux of $\sim $220 mJy is resolved out. This is likely the main cause for the seemingly inverted spectra when comparing the EVN 6 cm with the VLA 1.3 cm flux densities.

References

 
Copyright ESO 2007