Issue 
A&A
Volume 549, January 2013



Article Number  A139  
Number of page(s)  12  
Section  Extragalactic astronomy  
DOI  https://doi.org/10.1051/00046361/201118709  
Published online  16 January 2013 
Spectroastrometry of rotating gas disks for the detection of supermassive black holes in galactic nuclei
III. CRIRES observations of the Circinus galaxy^{⋆,}^{⋆⋆}
^{1}
Dipartimento di Fisica e AstronomiaUniversità degli Studi di
Firenze,
Firenze,
Italy
email: gnerucci@arcetri.astro.it; marconi@arcetri.astro.it
^{2}
INAF – Osservatorio Astronomico di Torino, Strada Osservatorio
20, 10025
Pino Torinese,
Italy
email: capetti@oato.inaf.it
^{3}
Physics Department, Rochester Institute of
Technology, 85 Lomb Memorial
Drive, Rochester,
NY
14623,
USA
email: djasps@rit.edu; axrsps]@rit.edu
^{4}
School of Mathematical & Physical Sciences, University of
Sussex, Falmer,
Brighton, BN2 9BH, UK
Received: 22 December 2011
Accepted: 3 November 2012
We present new CRIRES spectroscopic observations of the Brγ emission line in the nuclear region of the Circinus galaxy, obtained with the aim of measuring the black hole (BH) mass with the spectroastrometric technique. The Circinus galaxy is an ideal benchmark for the spectroastrometric technique given its proximity and secure BH measurement obtained with the observation of its nuclear H_{2}O maser disk. The kinematical data have been analyzed both with the classical method based on the analysis of the rotation curves and with the new method developed by us that is based on spectroastrometry. The classical method indicates that the gas disk rotates in a gravitational potential resulting from an extended stellar mass distribution and a spatially unresolved dynamical mass of (1.7 ± 0.2) × 10^{7} M_{⊙}, concentrated within r < 7 pc, corresponding to the seeinglimited resolution of the observations. The new method is capable of probing the gas rotation at scales that are a factor ~3.5 smaller than those probed by the rotation curve analysis, highlighting the potential of spectroastrometry. The dynamical mass, which is spatially unresolved with the spectroastrometric method, is a factor ~2 smaller, 7.9^{+1.4}_{1.1} × 10^{6}M_{⊙}, indicating that spectroastrometry has been able to spatially resolve the nuclear mass distribution down to 2 pc scales. This unresolved mass is still a factor ~4.5 larger than the BH mass measurement obtained with the H_{2}O maser emission, indicating that even with spectroastrometry, it has not been possible to resolve the sphere of influence of the BH. Based on literature data, this spatially unresolved dynamical mass distribution is likely dominated by warm molecular gas and has been tentatively identified with the circumnuclear torus that prevents a direct view of the central BH in Circinus. This mass distribution, with a size of ~2 pc, is similar in shape to that of the star cluster of the Milky Way, suggesting that a molecular torus, forming stars at a high rate, might be the earlier evolutionary stage of the nuclear star clusters that are common in latetype spirals.
Key words: techniques: high angular resolution / techniques: spectroscopic / galaxies: active / quasars: individual: Circinus / galaxies: kinematics and dynamics / galaxies: nuclei
Based on observations made with ESO Telescopes at the Paranal Observatory under programme ID 383.B0267(A).
Reduced spectral images are only available at the CDS via anonymous ftp to cdsarc.ustrasbg.fr (130.79.128.5) or via http://cdsarc.ustrasbg.fr/vizbin/qcat?J/A+A/549/A139
© ESO, 2013
1. Introduction
One of the fundamental as yet unresolved problems of modern astrophysics relates to the formation and evolution of the complex structures that characterize the presentday universe, such as galaxies and clusters of galaxies. Understanding how galaxies formed and how they become the complex systems we observe today is therefore a current major theoretical and observational effort.
There is now strong evidence for the existence of a connection between supermassive black holes (BHs), nuclear activity, and galaxy evolution. This evidence, which reveals the socalled coevolution of black holes and their host galaxies, is provided by the discovery of “relic” BHs in the center of most nearby galaxies, and by the tight scaling relations between BH mass (M_{BH} ~ 10^{6}−10^{10} M_{⊙}) and the structural parameters of the host spheroids such as mass, luminosity, and stellar velocity dispersion (e.g. Kormendy & Richstone 1995; Gebhardt et al. 2000; Ferrarese & Merritt 2000; Marconi & Hunt 2003; Häring & Rix 2004; Ferrarese & Ford 2005; Graham 2008a). Moreover, while it has long been widely accepted that active galactic nuclei (AGN) are powered by accretion of matter onto a supermassive BH, it has recently been possible to show that BH growth is mostly due to accretion of matter during AGN activity, and therefore that most galaxies went through a phase of strong nuclear activity (Soltan 1982; Yu & Tremaine 2002; Marconi et al. 2004). It is believed that the physical mechanism responsible for this coevolution of BHs and their host galaxies is probably feedback by the AGN, i.e. the accreting BH, on the host galaxy (Silk & Rees 1998; Fabian & Iwasawa 1999; Granato et al. 2004; Di Matteo et al. 2005; Menci 2006; Bower et al. 2006). Because the scaling relations between BH mass and host galaxy properties represent the clearest sign of coevolution, it is important to secure these relations by increasing the number, accuracy, and mass range of M_{BH} measurements.
Supermassive BHs are detected and their masses measured by studying the kinematics of gas or stars in galaxy nuclei. Currently, there are about ~50 BH mass measurements, most of which are in the ~10^{7}−10^{9} M_{⊙} range (e.g. Sani et al. 2010). The majority of these measurements have been made with longslit spectroscopy, but the development in recent years of integral field unit (IFU) spectrographs has resulted in an improvement in accuracy and reliability (see, e.g., Davies et al. 2006; Nowak et al. 2007, 2010; Krajnović et al. 2007, 2009; Cappellari et al. 2009; Neumayer et al. 2010; Rusli et al. 2011) of the mass determinations. One crucial issue in BH mass measurements is spatial resolution: a necessary but not sufficient condition is that the spatial resolution must be high enough to make it possible to spatially resolve the central regions of the galaxy, where the gravitational effects of the BH dominate those of the host galaxy (the socalled sphere of influence of the black hole). Even with the advent of adaptive optics (AO) assisted observations the best spatial resolutions achievable are ~0.1″, which corresponds to ~10 pc at a distance of 20 Mpc.
We have developed a new method based on the technique of spectroastrometry, which allows gas kinematical BH mass measurements that partly overcome the spatial resolution limitations of the “classical” gas (or stellar) kinematical methods. This method has been presented and discussed in detail by Gnerucci et al. (2010, 2011, hereafter G10, G11), and provides a simple but accurate way to estimate BH masses using either longslit or IFU spectra.
In this paper we apply this spectroastrometric method in an attempt to estimate the mass of the nuclear BH in the Circinus galaxy and to test whether it is possible to resolve the BH sphere of influence. At a distance of 4.2 Mpc (hence 1″ ≃ 20 pc), this is one of the closest Seyfert 2 galaxies (Freeman et al. 1977). Its nuclear activity is indicated by the observed line ratios (Oliva et al. 1994), by the ionization cone observed in [O III] (Marconi et al. 1994) and [Si VII] (Prieto et al. 2005), by the narrow coronal lines (Oliva et al. 1994; Maiolino et al. 2000), and by the broad (FWHM > 3300 km s^{1}) Hα emission in polarized light (Oliva et al. 1998). The discovery of H_{2}O maser emission, whose kinematics are indicative of a circularly rotating nuclear disk, has made possible one of the most impressive and accurate mass measurements (1.7 ± 0.3) × 10^{6} M_{⊙} (Greenhill et al. 2003b,a) of a supermassive BH to date. The relatively low BH mass makes the gravitational sphere of influence of the BH very small and spatially unresolved even with AO observations at 8 mclass telescopes. These two facts combined make this galaxy a very interesting benchmark to test the potential of the spectroastrometric approach.
Here we present new longslit spectra of the nuclear region of Circinus obtained with CRIRES at the ESO VLT. This instrument provides a very high spectral resolution that is essential to disentangle the relatively low gas velocities expected due to the relatively low BH mass estimated by Greenhill et al. (2003a). We perform two parallel analyses and model the CRIRES spectra using both the classical rotation curves approach and the spectroastrometric method, enabling us to check the quality of the modeling and to put tight constraints on M_{BH} based on a comparison of the independent results. In Sect. 2 we briefly review the key results of G10 and G11 on the application of spectroastrometry to rotating gas disks to enable the detection of nuclear BHs. In Sect. 3 we present the new CRIRES observations together with details of the data reduction and subsequent analysis. In Sect. 4 we describe the CRIRES Circinus gas rotation curves and their modeling. In Sect. 5 we present the matching spectroastrometric analysis and modeling of the CRIRES spectra. We compare and discuss the results from the spectroastrometric and rotation curves analyses in Sect. 6, with the aim of mutually constraining the two approaches. Finally, in Sect. 7 we discuss the results and draw our conclusions.
2. Spectroastrometric measurements of black holes masses
The spectroastrometric method (see Bailey 1998) consists of measuring the photocenter of emission lines in different wavelength or velocity channels. It has been used by several authors to study premainsequence binaries and inflows, outflows, or the disk structure of the gas surrounding premainsequence stars (Takami et al. 2003; Baines et al. 2004; Porter et al. 2004, 2005; Whelan et al. 2005).
In Gnerucci et al. 2010 (G10) we illustrated how the technique of spectroastrometry can be used to measure black hole masses at the center of galaxies. In that paper we focused on explaining the basis of the spectroastrometric approach and presented an extended and detailed set of simulations showing how this method can be used to probe the principal dynamical parameters of a nuclear gas disk. A key aspect of G10 was the comparison of this technique with the standard method for gas kinematical studies based on the gas rotation curve. We demonstrated that the two methods are complementary approaches to the analysis of spectral data (i.e. the former measures mean positions for given spectrum velocity channels while the latter measures mean velocities for given slit position channels). The principal limit of the rotation curves method resides in the ability to spatially resolve the region where the gravitational potential of the BH dominates with respect to the contribution of the stars. In G10 we demonstrated that spectroastrometry has the ability to provide information on the galaxy gravitational potential at scales significantly smaller than the spatial resolution of the observations (potentially reaching ~1/10). This fundamental feature can be illustrated by the following simple example: consider two pointlike sources located at a distance significantly smaller than the spatial resolution of the observations; these sources will be seen as spatially unresolved with their relative distance not measurable from a conventional image. However, if spectral features, such as absorption or emission lines, are present at different wavelengths in the spectra of the two sources, the spatial profiles of the light distribution extracted at these wavelengths will have different centroids, revealing the presence of the two sources. The separation between the sources can be estimated from the difference in the centroid positions at the wavelengths of the different spectral features, even if the separation is much smaller that the spatial resolution. Thus, the spectral separation of the two sources makes it possible to overcome the spatial resolution limit.
For clarity, we summarize here the principal features and the main steps of the method presented and discussed extensively in G10.

From the longslit spectrum of a continuumsubtracted emissionline one constructs the spectroastrometric curve by measuringthe line centroid along the slit for all wavelength channels. Thespectroastrometric curve of the line is given by the positioncentroids as a function of wavelength.

From the simulations presented in G10, we showed that the information about the BH gravitational field is predominantly encoded in the high velocity (HV) range of the spectroastrometric curve, which comprises the points in the red and blue wings of the line. In the case of Keplerian rotation, the HV part of the line spectrum originates from gas moving at high velocities closer to the BH; this emission is spatially unresolved. For this reason the HV part of the line spectrum is not strongly influenced by the spatial resolution or other instrumental effects such as slit losses or by the intrinsic line flux distribution. On the other hand, low velocity emission (hereafter LV) is usually spatially resolved (i.e. the gas moving at lower velocities is located farther away from the BH), so the spectroastrometric curve in this regime is not useful for the purpose of measuring the BH mass. The HV range of the curve is identified by measuring the spatial extent of the line emission as a function of wavelength and discarding the central (i.e. LV range) bins where the spatial profile becomes broader than the instrumental spatial resolution.

By measuring the spectroastrometric curves of a given line from at least three spectra taken at different slit position angles, one can obtain a spectroastrometric map of the source on the plane of the sky by geometrically combining the three curves. For integral field spectra, this step is obviously not necessary because the spectroastrometric map is derived directly from the data cubes. For a rotating disk with a radially symmetric line flux distribution the points of the spectroastrometric map should lie on the disk line of nodes. However, even for IFU data the effect of slit losses or a nonsymmetric line flux distribution can perturb the light centroid positions and move them away from the disk line of nodes. As shown in G10 and discussed above, these effects become negligible for the HV range of the map where the emission is spatially unresolved. In contrast, the LV points of the map tend to lie away from the line of nodes in a typical loop shape. The final spectroastrometric map is then obtained by selecting only the HV points.

One can then estimate the disk line of nodes by a linear fit to the HV range of the spectroastrometric map, project those points on the estimated disk line of nodes and obtain the disk rotation curve. Finally, one can apply a simple modelfitting procedure to obtain the parameters determining the gas rotation curve, and in particular the BH mass.
In a subsequent work (Gnerucci et al. 2011, G11), we applied the method to the radio galaxy Centaurus A, using seeinglimited longslit spectra and both seeinglimited and AOassisted IFU spectra. We selected this galaxy because it has been extensively studied using the gas kinematical method; the observed kinematics show that the gas is circularly rotating around the BH and that the mass and the disk parameters are well constrained. Moreover, both longslit and IFU data with different spatial resolutions are available, allowing a direct comparison of the spectroastrometry results to the results obtained from data sets with different characteristics. We demonstrated with real data that the method provides the same mass estimates as the classical gas kinematical method, but allows smaller spatial scales to be probed .
We briefly summarize the key results of G11 here.

We demonstrated with real data the capability ofspectroastrometry to overcome the spatial resolution limit. Theminimum distance from the BH at which we can measure the gasrotation curve is ~20 mas, which corresponds to ~1/15 of the spatial resolution for the seeinglimited data and ~1/6 for the AOassisted data.

The method based on spectroastrometry agrees excellently with the classical method that is based on the rotation curves (the BH mass estimates are consistent within ±0.2 dex and within less than ±0.05 dex when comparing the results obtained from the same dataset). This demonstrates the robustness of the method: using the same dataset, we can independently apply the classical and the spectroastrometric methods and obtain consistent results.

The application of the spectroastrometric method to different types of data (IFU and longslit) gives consistent results (within only ~0.1 dex), demonstrating the versatility of our method.

A typical feature of spectroastrometry is its insensitivity to disk inclination. In our modeling, mass and disk inclination are in fact coupled. Therefore our method can return only a value for M_{BH} sin^{2}i; the inclination must be assumed or determined by another method to derive the value of the mass.

The spectroastrometric method was applied independently of the classical method. However, as discussed in G10, it is clear that the spectroastrometric and classical rotation curves are complementary and orthogonal descriptions of the position velocity diagram. Therefore, a development of this method will be its application in combination with the classical method based on rotation curves. This provides constraints on the disk inclination and thus removes the massinclination degeneracy.
The utility of the method is not limited to gas disks rotating around supermassive black holes but also to galaxy disks. Indeed, we have applied the method to improve virial mass estimates of highz galaxies observed with IFU spectra (for more details see Gnerucci et al. 2011a).
Fig. 1 Continuumsubtracted detector 3 CRIRES spectrum (slit PA1) extracted at the position of the continuum peak. Solid red line: fit to Brγ using a GaussHermite function. 
Fig. 2 Rotation curves for the CRIRES Brγ spectra. Left panel: slit PA1. Central panel: slit PA2. Right panel: slit PA3. The solid red lines represent the curves expected from the model. 
3. Observations and data reduction
Circinus was observed between April and July 2009 (program 383.B0267A) with CRIRES (Cryogenic highresolution Infrared Echelle Spectrograph; Kaeufl et al. 2004) at the ESO VLT with the aid of the MACAO (Multi Applications Curvature Adaptive Optics) adaptive optic system. The observations consist of three nuclear spectra characterized by a different slit position angle: the slits with position angles of 30°, 90°, and 150° with respect to the north direction are denoted by PA1, PA2, and PA3. The orientation of PA1 was chosen to align the slit with the major axis of the galaxy, and PA2 and PA3 were incrementally rotated by 60° to provide a uniform coverage in position angles with the available slits.
The AO module MACAO was used with the unresolved Circinus nucleus as a guide star. The spectra were obtained with a 0.4″ wide slit (slit length ~31″) and a resolving power of λ/Δλ = 50 000, corresponding to a spectral resolution of ~0.4 Å (~5.5 km s^{1}) at the observed Brγ wavelength (2.169 μm). The resulting wavelength range is ~2.137−2.188 μm, covered with a mosaic of four InSb arrays that provide an effective 4096 × 512 focal plane detector array in the focal plane. The choice of the very high spectral resolution is critical for the measurement of the low velocities and velocity dispersions that are expected, given the relatively low BH mass (Greenhill et al. 2003a). The detector pixel scale is 0.086″/pixel along the slit axis and 0.102 Å/pixel along the dispersion direction. For each position angle we obtained six spectra with an exposure of 180 s, nodding the target along the slit for sky subtraction, which results in a total onsource exposure of 1080 s.
The data were reduced using the CRIRES reduction pipeline (version 1.8) to subtract dark frames, flatfield correction, sky subtraction, wavelength calibration and to combine the various observing blocks. IRAF tasks^{1} were then used to rectify the spectra and correct for telluric absorption using a suitable standard star. During data reduction, we concentrated only on the third detector that targeted the Brγ line (rest frame wavelength 2.1661 μm) observed at ~2.169 μm. The spatial resolution of the data was estimated in the final reduced spectra from the extension of the nuclear continuum along the slit (the galaxy nucleus with an estimated size of 1.9 ± 0.6 pc, corresponding to at 3.5 Mpc, is in fact unresolved at the spatial resolution of these observations; Prieto et al. 2004). We obtain an average value of ~0.7″ FWHM for the spectra at the three PAs, indicating that the AO correction did not perform well, probably due to the non pointlike nature of the Circinus nucleus in the R band. The spectra were continuumsubtracted since, as discussed in G10 and G11, the spectroastrometric analysis requires a continuumsubtracted spectrum. Finally, because the dispersion was higher than needed (~1.4 km s^{1}/pixel at Brγ), we rebinned the spectra by 5 pixels along the dispersion direction to improve the signaltonoise ratio (S/N).
The final continuumsubtracted Brγ spectra have a typical S/N ~ 35. This value is obtained from the nuclear spectrum extracted from an aperture along the slit equal to the spatial resolution; the Brγ profile is fitted with a GaussHermite model (see below) and the quoted S/N is defined by the ratio between the peak model value and the rms of the fit residuals.
With our observational setup (10 km s^{1} spectral resolution, 07 spatial resolution) the minimum detectable BH mass is determined by the spatial resolution and the thermal broadening of the ionized gas (i.e. σ ~ 15−22 km s^{1} for T_{e} = (1−2) × 10^{4} K), and corresponds to (1)if is the spatial scale probed with spectroastrometry. At this stage, this is a purely indicative value.
Fig. 3 Surface brightness profiles of the Brγ line along the slits (black lines). The red lines represent the surface brightness of the underlying continuum. 
Fig. 4 Upper panel: fit of the NICMOS F222m light profile. The black continuous line represents the bestfit model. The dotdashed line represents the profile of the compact component ( FWHM size) and the dashed line the extended component. The compact component is detected and identified with hot dust emission in NACO observations by Prieto et al. (2004). The spatial extension of the compact component is similar to that of the NICMOS PSF and therefore the first Airy ring is still visible. Lower panel: model residuals. 
4. Analysis of the rotation curves
We measured the gas rotation curves in the three spectra (PA1, PA2, and PA3) by fitting the Brγ line row by row along the slit direction with a GaussHermite profile (Cappellari & Emsellem 2004) thus obtaining mean velocity, velocity dispersion, and line flux at each position along the slit. In Fig. 1 we show a fit example corresponding to the PA1 continuumsubtracted spectrum, rebinned by 5 pixels along the dispersion direction and extracted from one pixel along the slit at the position of the continuum peak. The rotation curves obtained at the three slitposition angles are presented in Fig. 2 and clearly show the typical Slike shapes expected from rotating disks. Fig. 3 shows the Brγ surface brightness profiles along the slits (black lines) compared with the corresponding continuum curves (red lines). Since continuum emission is dominated by the unresolved hot dust emission at the spatial resolution of our observations (Prieto et al. 2004), Figs. 3 and 2 clearly show that we spatially resolve the emission regions and the kinematics of Brγ.
The rotation curves are first analyzed according to the classical gas kinematical method. The modeling of the rotation curves is performed following the procedure first described by Macchetto et al. (1997) and subsequently refined by several authors; here we used the modeling code described in detail by Marconi et al. (2003, 2006). Very briefly, the code computes the rotation curves of the gas assuming that the gas is rotating in circular orbits within a thin disk in the principal plane of the galaxy potential. We neglect any hydrodynamical effect such as gas pressure. The gravitational potential consists of two components: the stellar potential, characterized by its masstolight ratio M/L, and a spatially unresolved mass concentration characterized by its total mass M_{UDM} (UDM means unresolved dynamical mass). This spatially unresolved dynamical mass concentration is dark in the sense that it is not accounted for by the continuum emission used to trace the stellar mass distribution. It could represent the putative supermassive black hole but also any spatially unresolved stellar or gaseous component or a combination of them. In computing the rotation curves we took into account the finite spatial resolution of the observations, the intrinsic surface brightness distribution (ISBD) of the emission lines, and we integrated over the slit and pixel area. The free parameters characterizing the bestfitting model are found by standard χ^{2} minimization.
We first determined the stellar gravitational potential from a Kband surface brightness profile of the Circinus galaxy that was obtained from a NICMOS/CAMERA2 F222M mosaic kindly provided by Roberto Maiolino (for details on observations and data reduction see Maiolino et al. 2000). The inversion procedure to derive the stellar density distribution from the surface brightness is not unique if the gravitational potential does not have spherical symmetry. Assuming that the gravitational potential is an oblate spheroid, the inversion requires knowledge of the potential axial ratio q and the inclination of its principal plane with respect to the line of sight, i. These two quantities are related by the observed isophote ellipticity, and for the Circinus galaxy we solved this ambiguity by imposing an axial ratio of ~0.1 that corresponds to an almost disklike spheroid; Circinus is in fact an SA(s)b spiral galaxy and, moreover, the stellar contribution to the gravitational potential is maximized by imposing a disklike geometry. Following van der Marel & van den Bosch (1998), we then converted the oblate spheroid density distribution model to an observed surface brightness distribution in the plane of the sky by integrating along the line of sight, convolving with the point spread function (PSF) of the telescope+instrument system and averaging over the detector pixel size. Then, the derived model light profile can be directly compared with the observed one. A detailed description of the relevant formulae and the inversion and fit procedure is presented in Marconi et al. (2003). The results of the analysis of the NICMOS F222M profile are presented in Fig. 4. In the upper panel the black solid line represents the model surface brightness profile convolved for the instrumental effects. This model profile is the combination of an extended and a compact components, represented by dashed and dotdashed lines, respectively. The extended component represents stellar emission and is parameterized with the oblate spheroid described above. The compact component is characterized by spherical symmetry and by a sharp boundary, resulting in an FWHM of . This component is consistent with the compact Kband source of size ~ detected with NACO by Prieto et al. (2004) and identified with hot dust emission from the AGN torus on the basis of the steep nearIR colors. This identification has also been confirmed by Müller Sanchez et al. (2006), who were able to deconvolve the stellar and dust continua, confirming that the compact Kband emission is dominated by hot dust. Therefore we did not consider it for the stellar mass profile used in the analysis of the rotation curves.
The bestfitting rotating disk model is represented in Fig. 2 by the red solid line and, overall, it nicely reproduces the observed rotation curves. One possible cause of concern is that the rotation curve at PA3 shows an ~50 km s^{1} velocity shift with respect to the rotating disk model and, indeed, the red line in the right panel of Fig. 2 has been offset by the same amount to match the observed points. PA3, with a position angle of 150°, is almost perpendicular to the line of nodes, which approximately aligns with the PA1 slit (PA 30°). This shift might then be accounted for by outflowing motions because the PA3 slit is lying within the ionization cone illuminated by the central AGN. Such outflows are commonly observed in Seyfert galaxies and are likely driven by AGN radiation pressure or winds (e.g. MüllerSanchez et al. 2011 and references therein). However, since the rotation curves from the PA1 and PA2 slits are both well reproduced by a rotating disk model and since, after allowing for the velocity shift, the PA3 slit rotation curve is also well reproduced by the same model, we believe that the outflowing motions detected in PA3 do not affect the final mass estimate, similarly to what has been found in Cygnus A (Tadhunter et al. 2003).
Since the disk inclination is coupled with the unresolved dynamical mass (i.e. M_{UDM} and stellar M/L ratio, see, e.g., Marconi et al. 2006), we chose to keep it as a fixed parameter in the modeling to avoid convergence problems with the χ^{2} minimization. Its best value and confidence interval is then identified by using a grid of fixed i values and performing the fit for each of them. In this way we constructed the χ^{2} vs. i curve shown in Fig. 5, which allows us to identify both the best i value and the confidence intervals (for details see Avni 1976). The best inclination value and confidence interval (at 1σ confidence level) is (61 ± 1)°. This value agrees well with the value of 65° recovered by Freeman et al. (1977) from largescale optical photometry and with the value of 55° obtained by Hicks et al. (2009) for the inner H_{2} gas disk (radius ≲9 pc).
Fig. 5 χ^{2} vs. i curve for the determination of best value and confidence interval of the disk inclination. The dotted lines represents the 1, 2, and 3σ confidence levels. 
The bestfit model parameters for the Brγ rotation curves are reported in Table 1, while in Fig. 2 we show the Brγ rotation curves and the relative bestfit model. We estimate the uncertainties on the bestfit model parameters using the bootstrap method (Efron & Tibshirani 1994). The dataset consists of 181 elements in total from the rotation curves of the three slits, each characterized by spatial position, flux, velocity, and velocity dispersion. We randomly extracted from this dataset a subsample with the same number of elements. Due to the random extraction, each subsample will have some elements replicated a few times and some elements that are entirely missing. We then performed the fit on these randomly extracted 100 subsamples and estimated errors on parameters by taking the standard deviation of the bestfit values, which are usually normally distributed.
Since M_{UDM} and M/L are correlated, we also evaluated the confidence intervals for the coupled distribution of these two model parameters. To accomplish this, we constructed a grid of values in the M_{UDM} − M/L plane and performed the fit for each of these points by varying all other parameters. In this way we created a χ^{2} surface that allows us to identify both the best values and the confidence regions in the M_{UDM} − M/L plane (for details see Avni 1976). In Fig. 6 we show the resulting contours of the confidence regions. Each contour is labeled with the corresponding confidence level. As shown in the figure, the confidence regions are consistent with the statistical uncertainties obtained with the bootstrap method for these parameters (cf. Table 1), and the M_{UDM} and M/L parameters show the expected anticorrelation.
Fig. 6 Confidence regions in the M_{UDM}M/L plane for the rotation curve model fits. The isocontours indicate the 95%, 90%, and 68% (the inner one) confidence levels. The dotted line marks the M_{UDM}M/L values corresponding to the minimum χ^{2} fit. The open circles indicate the grid of values used in the M_{UDM}M/L plane. 
5. Spectroastrometric analysis
5.1. Analysis of the spectra
As discussed in G10 and G11, to reduce the effects of noise in measuring the spectroastrometric curves, we constructed a synthetic position velocity diagram (PVD) of the Brγ line for each longslit spectrum. We fitted the Brγ line with a GaussHermite function at all positions along each of the PA1, PA2 and PA3 slits, obtaining the relative model parameters (flux, mean velocity, velocity dispersion, and Hermite parameters h_{3} and h_{4}). We then used the fitted profiles of Brγ to reconstruct noisefree synthetic PVDs for each slit.
The PVD for the original Brγ longslit spectrum at PA1 is compared with its synthetic version in Fig. 7. It can be seen that the synthetic PVD is noisefree because each row represents the fitted parametric profile. However, one has to take into account the errors on the fitted parameters to estimate the errors on the synthetic pixel counts. For each spectral fit we therefore simulated 1000 synthetic spectra from 1000 realizations of the set of the five profile parameters distributed following a pentavariate distribution with the fit correlation matrix. The flux and error of each pixel was then estimated from the mean and standard deviation of the 1000 realizations. We note that for each flux profile along the slit the errors on fluxes are uncorrelated because they originate from independent fits to the line profiles.
Fig. 7 Position velocity diagram of the continuumsubtracted Brγ spectrum at PA1. Upper panel: observed spectrum. Bottom panel: synthetic reconstruction. The horizontal dotted line overplotted on each panel represents the continuum peak position. The isophotes denote the same values in both panels. 
Fig. 8 Spectroastrometric curves of the Brγ line at the three slit position angles. Left panel: PA1. Central panel: PA2. Right panel: PA3. The dashed vertical lines in each panel represent the limits of the HV range. Wavelengths are converted into velocity using as reference (zero velocity) the rest frame Brγ wavelength (2.1661 μm). 
From the synthetic Brγ spectra for the three slits (PA1, PA2, and PA3), obtained following the method outlined above, one can derive the spectroastrometric curves that are shown in Fig. 8.
From Fig. 8 we can see that the position of the light centroids in the highvelocity (HV) range tend to approach the 0 position (i.e. the position of the continuum peak). As discussed in G10 and G11, this is the expected behavior of spectroastrometric curves in the presence of an unresolved central mass (i.e. the BH). This behavior is less evident on the red side because of the small number of HV points. Errors on photocenter positions range from ~0.02″ to ~0.1″, that is, from ~1/35 to ~1/5 of the spatial resolution of the data; this is the accuracy with which we can measure centroid positions.
5.2. The spectroastrometric map of the source
We obtained three spectroastrometric curves from Brγ, one for each PA of the slit. Each spectroastrometric curve provides the photocenter position along one slit, i.e. the position of the photocenter projected along the axis defined by the slit direction. Thus, combining the spectroastrometric curves obtained at different PA, we can obtain the map of photocenter positions on the plane of the sky for each velocity bin. In principle, the spectroastrometric curves from two nonparallel slits should suffice but we can use the redundant information from the three slits to recover the 2D sky map as described in Sect. 4.1 of G10. We have chosen a reference frame in the plane of the sky centered on the center of the PA1 slit (which corresponds to the position of the continuum peak along the slit) with the X axis along the north direction. For a given velocity bin we then determined the position of the light centroid on the sky plane, producing the 2D spectroastrometric map shown in Fig. 9.
As discussed in G10 and G11, the coordinates on the plane of the sky of the center of the PA2 and PA3 slits must be considered as free parameters. These unknowns are estimated simultaneously with the position of the photocenter following a χ^{2} minimization procedure. The final spectroastrometric map on the plane of the sky is that given by the bestfitting set of slit centers. The error bars on the points represent the uncertainties resulting from the fit. The black points correspond to the HV points (i.e. v ≲ 295 km s^{1} and v ≳ 475 km s^{1}) that were actually used to determine the location of the slit centers. The HV parts of the line profile represent the tails of the lineofsight velocity distribution and could not be selected by identifying spatially unresolved emission along the slit, i.e. the criterion adopted in G11, since emission along the slit direction is spatially resolved. We therefore extracted a spectrum of the Brγ line by averaging the CRIRES spectrum over an aperture equal to the spatial resolution and centered on the continuum peak and selected the velocity bins characterized by a flux lower than 0.3 times the line peak flux. This criterion for identifying the HV range is different from the one used in G11 for the Centaurus A spectra. However, it produces the same HV range for Centaurus A and is therefore equivalent. The spatial extension of the emission in the HV region most probably indicates that the HV spectroastrometric measurement probes the gravitational potential of an extended mass distribution rather than that of the BH. This question will be discussed below, where we will show that, indeed, the spectroastrometric analysis indicates the presence of an extended mass distribution. The emission of the gas moving at higher velocities does not originate from the inner region of the disk that rotates around the BH but feels the gravitational potential of an extended mass component.
The 2D spectroastrometric map just described (and shown in Fig. 9) can now be used to estimate the geometrical parameters of the nuclear gas disk. If the gas kinematics are dominated by rotation around a pointlike mass (M_{UDM}), the position of the light centroid at the high velocities should lie on a straight line (which identifies the direction of the disk line of nodes) and should approach, at increasing velocities, the position of the rotation center. This consideration allows us to make a first estimate of the position on the plane of the sky of the rotation center as the average position of the HV points in the 2D spectroastrometric map^{2} as well as the position angle of the line of nodes (θ_{LON}), obtained by fitting a straight line to the HV points (see Fig. 9). A more accurate estimate of these parameters, derived from the model fitting, is described in the next section (see Table 1). The uncertainty on the center position is ~0.04″, i.e. ~1/18 of the spatial resolution of the data.
Fig. 9 2D spectroastrometric map for the Brγ line. The red point marks the inferred position of the pointlike mass. The red solid line represents the line of nodes of the disk obtained from a linear fit to the HV points, as described in the text. The dotted red lines represent the 1σ uncertainties on the position angle of line of nodes. The origin of the map is the position on the sky plane of the PA1 slit center (which corresponds to the continuum peak position). 
5.3. Estimate of the unresolved mass from the spectroastrometric map
We recovered the value of the pointlike mass from the spectroastrometric map, following the method presented and discussed in detail in G10 and G11.
Briefly, under the assumption that the gas lies in a thin disk configuration inclined by i with respect to the plane of the sky (i = 0 faceon) and the disk line of nodes has a position angle θ_{LON}, the line of sight component of the circular velocity of a gas particle with distance r from the rotation center (hereafter V_{ch} for channel velocity) is given by (2)where L(r) is the radial luminosity density distribution in the galactic nucleus, M/L is the masstolight ratio of the stars, and we also added the systemic velocity of the galaxy V_{sys}.
Fig. 10 Results of the fit to the spectroastrometric Brγ data. The left panel shows the rotation curve projected along the line of nodes, S_{ch} vs. V_{ch}. The right panel shows the r = S_{ch} − S_{0} vs. V = V_{ch} − V_{sys} rotation curve. The solid red lines represent the curves expected from the model. The dotted line in right panel represents the rotation curve due to the star component of the gravitational potential. 
First we recovered the disk line of nodes by fitting a straight line on the 2D map. Then we projected the position of the 2D map points (x_{ch},y_{ch}) on the line of nodes, calculating their coordinate with respect to this reference axis (S_{ch}) and then their distance r from the rotation center used in Eq. (2) (i.e. r = kS_{ch} − S_{0} where S_{0} is the coordinate along the line of nodes of the disk and k is a scale factor to transform angular to linear distances^{3}; see G10 for details).
The unknown parameters of this model are found by minimizing the quantity (3)where Δ(S_{ch};par) is the uncertainty of the numerator. As previously discussed, we restricted the fit (i.e. the sum over the velocity channels) to the HV range of the map. The channel velocity V_{chan} has no associated uncertainty since it is not a measured quantity, but the central value of the velocity bin. Finally we added a constant error (Δ_{sys}) in quadrature to the quantity Δ(S_{ch};par) to obtain a reduced χ^{2} close to 1 (see Sect. 5 of G10 for a detailed explanation of this choice). Finally, using the bestfit values of the model parameters, we can compute the (x,y) position of the rotation center in the sky plane.
We verified that the value of M_{UDM} is little affected by the actual values of the position angle of the line of nodes and of S_{0}, the position of the rotation center along the line of nodes. Indeed, repeating the fit with θ_{LON} and S_{0} values randomly varied within the uncertainties, M_{UDM} changes by ~0.06 dex, consistently with the typical 1σ statistical uncertainties of the fit (see Table 1).
As discussed previously and in G10 and G11, disk inclination i and spatially unresolved mass concentration are coupled and this fitting method can only measure M_{UDM} sin^{2}i. Therefore, we assumed a value for the inclination to obtain a mass value. In the following, we consider a disk inclination i = 61°, as obtained in the rotation curve analysis. Summarizing, the free parameters of our fit are
The fit results are tabulated in Table 1 and presented graphically in Fig. 10, where we plot S_{ch} vs. V_{ch}, the rotation curve projected along the line of nodes, and r = S_{ch} − S_{0} vs. V = V_{ch} − V_{sys}. The solid red lines represent the curves expected from the model (S_{ch} vs. V_{ch}^{model} and r vs. V_{ch}^{model} − V_{sys}, respectively).
Fit results.
The first important result from this analysis is that the minimum distance from the rotation center where it is possible to make a velocity estimate is ~0.1″ corresponding to ~2.3 pc (see right panel of Fig. 10), while with the standard rotation curve method the minimum distance from the center that can be observed is about half the spatial resolution (~0.35″). This clearly shows how spectroastrometry can overcome the spatial resolution limit.
It is not possible to obtain measurements at spatial scales smaller than ~1/3 of those probed by the rotation curve analysis because of the limited S/N of the spectra; this prevents us from measuring the photocenters of the line at higher velocities, which would additionally extend the curves in Fig. 8 to the red and blue sides.
6. Comparison of the rotation curves and spectroastrometric analyses
Here we compare the results of the two independent analyses of the CRIRES spectra (i.e. the fits labeled FitR 0 and FitS 0 in Table 1) and discuss the combined constraints from the two methods. Finally, we reanalyze the data taking into account these combined constraints.
As discussed in G10 and G11, the modeling of the spectroastrometric data is not able to constrain the masstolight ratio M/L of the nuclear star distribution because it models the gas rotation curves at small distances from the rotation center where the contribution of the stellar mass to the gravitational potential is negligible. Indeed, performing a first model fit with M/L free to vary (FitS 0 in Table 1), we obtain a value of log _{10}(M/L) ≃ −11. Therefore we used the results of the rotation curve modeling to constrain this parameter. In the FitS 1 presented in Fig. 10 and Table 1 we fixed the M/L to the value obtained from the rotation curves analysis. Another important check concerns the geometrical parameters of the modeled gas disk (i.e. the position angle of the line of nodes θ_{LON} and the disk center, or equally, the center position on the plane of the sky (x_{c},y_{c})). The spectroastrometric model fitting gives a value of 217° for θ_{LON}. This is consistent with the rotation curve modeling, which gives a bestfit value of 215°. On the other hand, the rotation curve modeling gives a rotation center that is shifted south by ~0.05″ with respect to that returned by the spectroastrometric modeling. However, the spectroastrometric map probes a spatial region of radius ~0.2″, whereas the rotation curves probe distances up to ~3″ from the disk center; therefore, we expect the former to give a more robust indication of the center position than the latter.
Another constraint that the spectroastrometry can place on the rotation curves analysis is the position of the centers of the three slits on the plane of the sky. As previously described, when we combine the three spectroastrometric curves to obtain the spectroastrometric map, we obtain an estimate of the positions of the slit center with an accuracy better than that of the telescope pointing (see G10 and G11 for details).
Therefore, we repeated the rotation curve modeling imposing geometrical constraints obtained from the spectroastrometric analysis, namely the slit center positions and the values of θ_{LON} and (x_{c},y_{c}) (FitR 1 in Table 1). This produces a higher value of the reduced χ^{2} than the original fit (FitR 0 in Table 1). However, the bestfit M_{UDM} and M/L values are the same, within the uncertainties. The differences relative to the FitR 0 case (~− 0.03 dex and of + 0.03 dex, for M_{UDM} and M/L, respectively; Table 1) can be considered an indication of the influence of the geometrical disk parameters on the derived M_{UDM} and M/L values.
The slightly poorer fit quality of FitR 1 may also be an indication that the inner disk probed by the spectroastrometric analysis has a different geometry (in this particular case the disk geometrical center position) than the outer disk, which influences the rotation curves. The rotation curves probe the average disk geometric parameters over a spatial region that extends over the central ~100 pc, whereas spectroastrometry probes the inner ~10 pc.
Regarding the principal parameter of the modeling, M_{UDM}, we note that the rotation curve fits give a mass estimate higher by ≈ 0.35 dex with respect to the values returned by the spectroastrometric modeling. This difference is larger than the statistical or systematic uncertainties, but the good agreement between the two modeling approaches with respect to the geometrical disk parameters gives confidence that the results of the fitting are robust. We therefore attribute the difference in M_{UDM} to the different spatial scales probed by the two methods. For the rotation curve approach, as previously noted, the spatial resolution of the observations sets the minimum radius at which the gas rotation curve can be probed. Therefore, we can only measure the total dynamical mass enclosed within a radius equal to half the spatial resolution with this approach, in this case corresponding to ~0.35″ or 7 pc. On the other hand, the spectroastrometric approach is able to probe the gas rotation curve at smaller radii, allowing us to measure the total dynamical mass enclosed within ~0.1″ (~2 pc, see Fig. 10). We conclude that the difference in the mass measured by the two approaches (7.6 × 10^{6} M_{⊙} from spectroastrometry and 1.7 × 10^{7} M_{⊙} from rotation curves) is most likely due to an extended mass distribution within the inner ~0.35″ (7 pc), which is large compared to the BH mass (~1.7 × 10^{6} M_{⊙}).
Fig. 11 Dynamical mass measurements in the nuclear region of the Circinus galaxy. Measurements are marked by filled circles of different colors and are identified in the legend. The red filled circle represents the CRIRES spectroastrometry mass measurement obtained assuming a disk with i = 61° with respect to the line of sight, same as the largescale measurements; the open red circle represents the spectroastrometry mass measurement obtained assuming an edgeon disk, same as the maser disk. The region shaded by gray dotted lines is characterized by r < 20 mas and is the region probed by the H_{2}O maser rotation curve, where the dynamical mass is mostly unresolved and belongs to the BH. The enclosed mass within this region must be dominated by the BH, since no evidence for extended mass is seen in the maser rotation curve. The gray stripe represents the radial total mass distribution of the bestfit model for the CRIRES rotation curves (taking into account errors on M_{UDM} and M/L). The orange line represents the total mass distribution, which is a combination of BH mass, nuclear (4 pc size) and extended mass distribution, with the mass distribution derived by Müller Sanchez et al. (2006). The nuclear mass distribution corresponds to what we measure as M_{UDM}. The green line is similar to the orange line but the nuclear mass distribution now has a size of 2 pc. The dashed green line is the contribution of BH mass and nuclear mass distribution, while the dotted line represents the BH mass and the extended mass distribution. The continuous black line represents the radial mass distribution of the nuclear star cluster at the center of the Milky Way (Genzel et al. 2010) combined with the BH mass (Greenhill et al. 2003a) and rescaled to match the measurements at ~10 pc scale. 
7. Nuclear mass distribution
The most important result from our measuring of the mass of the BH in Circinus is that the M_{UDM} value estimated from rotation curve modeling is ~0.35 dex higher than the value estimated from spectroastrometric modeling. Moreover, the BH mass measured by Greenhill et al. 2003a from the H_{2}O maser spectroscopy (1.7 × 10^{6} M_{⊙}) is even lower (~0.7−1 dex) than our estimates. The analyses based on rotation curves and spectroastrometry can robustly probe gas rotation and thus the mass distribution at different distances from the dynamical center. The lower limits on these distances (limiting inner radii) are set by the instrumental setup. For the rotation curves the limiting inner radius is half the instrumental spatial resolution and corresponds to ~0.35″ or 7 pc for our Circinus data. For the spectroastrometric analysis the limiting inner radius is a fraction of the spatial resolution and corresponds to ~0.1″ or 2 pc (right panel of Fig. 10). Therefore the different measurements of the unresolved dynamical mass indicate an extended mass distribution, revealed by the different spatial scales. This extended mass distribution could not be identified in the Kband continuum light profile, also because of the presence of the strong hot dust emission within the inner 02 (Prieto et al. 2004). It was only revealed as unresolved mass in our dynamical analyses.
In Fig. 11 we summarize existing dynamical mass measurements performed in the nuclear region of the Circinus galaxy. The enclosed mass is plotted as a function of distance from the dynamical center, which is assumed to coincide with the BH location. The blue point represents the BH mass measurement by Greenhill et al. (2003a) from modeling of the H_{2}O maser rotation curve and is located at the inner radius probed by the maser rotation curves. The maser disk is seen almost edgeon. The gray region characterized by r < 20 mas is the region probed by the H_{2}O maser rotation curve, where the dynamical mass is mostly unresolved and belongs to the BH. The outer limit of this region is set by the maximum radius probed by the maser rotation curve. The red filled circle represents the CRIRES spectroastrometry mass measurement obtained assuming a disk with i = 61° with respect to the line of sight. This is the inclination that is determined from the analysis of the rotation curves at larger scales and is close to the inclination of the galactic disk. Since the scales probed by spectroastrometry are intermediate between those of the galactic and maser disks, we also considered the possibility that the spectroastrometry is probing rotation from an edgeon disk (open red circle). Clearly, even if the disk were seen edgeon, the observed kinematics at ~2 pcscales would still require an extended mass. The black circle represents the mass measurement from the CRIRES rotation curves and is located at half the spatial resolution. Finally, the brown and orange points represent measurements of dynamical masses enclosed in 8 pc and 9 pc radii by Müller Sanchez et al. (2006) and Hicks et al. (2009), respectively, using SINFONI AOassisted observations. It is clear that the measurements from SINFONI and CRIRES agree within the errors. The gray stripe represents the radial total mass distribution of the bestfit model for the CRIRES rotation curves (taking into account errors on M_{UDM} and M/L). This is the mass distribution one would have derived considering only the Kband surface brightness profile.
Inspection of Fig. 11 reveals a spatially extended mass distribution within the inner 10 pc of the nuclear region of Circinus. It also shows the capability of spectroastrometry to improve the spatial resolution by a factor ~3, providing constraints on the extended mass distribution but, unfortunately, it is still not possible to measure the BH mass. Indeed, the stellar mass distribution recovered from the NICMOS Kband continuum light profile does not account for the mass distribution in the inner 10 pc and leads to an overestimated unresolved dynamical mass.
The extended mass within 10 pc might be accounted for by stars not identified in the NICMOS image because of the hot dust emission or might be accounted for by cold gas. The AOassisted SINFONI observations by Müller Sanchez et al. (2006) provided the surface brightness profiles of hot dust and stellar emission, as well as those of Brγ and H_{2}. As shown in their Figs. 3 and 4, the stellar emission is more extended than the hot dust and gaseous components. Moreover, the stellar component is offset by ~ and its mass is ~10^{6} M_{⊙}, making it unlikely that M_{UDM} can be accounted for by stars whose emission is hidden in NICMOS by the strong hot dust emission. On the other hand, Müller Sanchez et al. (2006) found that Brγ and H_{2} surface brightness distributions are consistent with an exponential disk with scale radius r_{d} ≃ 4 pc. Moreover Müller Sanchez et al. (2006) found that the nuclear H_{2} luminosity corresponds to a molecular gas mass of 1.7 × 10^{7} M_{⊙}, fully consistent with the dynamical mass within 10 pc. Therefore the extended mass distribution within 10 pc might be accounted for by a disk of mostly molecular gas. To verify this hypothesis, we plot with an orange line in Fig. 11 the mass distribution obtained by considering the BH mass by Greenhill et al. (2003a), the stellar mass distribution from the NICMOS Kband surface brightness profile, and an exponential disk with r_{d} = 4 pc and mass 1.7 × 10^{7} M_{⊙}. This is consistent with the analysis of Müller Sanchez et al. (2006), but fails to reproduce our spectroastrometric measurements because this mass distribution is too extended. A much better agreement is found considering an exponential disk with r_{d} = 2 pc and mass 1.4 × 10^{7} M_{⊙}, which is shown by the green solid line. For comparison, the dashed and dotted green lines represent the relative contribution of the gas and stellar masses (each of them added to the BH mass). This is perfectly consistent with the results by Müller Sanchez et al. (2006) considering the uncertainties in converting the emission line surface brightness distributions in mass distribution.
The spectroastrometric measurements probing smaller scales thus indicate that the mass distribution is more concentrated than is inferred from the Brγ and H_{2} surface brightness distributions. The mass that is unresolved even by spectroastrometry has a high average density of 1.4 × 10^{5} M_{⊙} pc^{3} and is thus expected to host significant amounts of star formation. Indeed, (Müller Sanchez et al. 2006) found that significant star formation is ongoing within the central 8 pc and identified the molecular medium with the torus required by the AGN unified model that is believed to exist in the nucleus of Circinus, a Seyfert 2 galaxy.
From the green line it is also possible to infer that the contribution of gas and stars to the mass distribution equals that of the BH mass at ≃ 1 pc, which is then to be considered as the radius of the gravitational sphere of influence of the BH. This is perfectly consistent with the independent estimate based on the stellar velocity dispersion. For a stellar velocity dispersion of σ ≃ 75 km s^{1} (e.g., Graham 2008b) the sphere of influence is r_{BH} = GM_{BH}/σ^{2} = 1.2 pc, remarkably similar to our results here.
Finally, the black line represents the mass profile that is obtained by considering the BH mass and the star cluster in the Milky way (Genzel et al. 2010) with a mass rescaled to match the observed enclosed mass at 10 pc. Genzel et al. (2010) modeled the Milky way nuclear star cluster with a double power law density distribution characterized by a break radius of 0.25 pc, inner power law r^{1.3}, outer power law r^{1.8}, and density at the break radius 1.35 × 10^{6} M_{⊙} pc^{3}.
The comparison with the Milky Way is suggested by the similarity of morphological types between the two galaxies and indicates that, overall, the nuclear mass distributions at r < 10 pc scales are not significantly different. It is intriguing to think that, if the entire molecular gas in Circinus were converted into stars, it would produce a nuclear star cluster similar to that observed in the Milky way, which is also commonly observed in latetype spirals. Since the molecular material is likely associated with the torus invoked by the AGN unified model, it is also intriguing to speculate that there exists an evolutionary track in which dense nuclear molecular tori are converted into nuclear star clusters.
8. Conclusions
We have presented new CRIRES spectroscopic observations of the Brγ emission line in the nuclear region of the Circinus galaxy, obtained with the aim of measuring the BH mass using the spectroastrometric technique. The Circinus galaxy is an ideal benchmark for the spectroastrometric technique, given its proximity and a secure BH measurement obtained from observations of the nuclear H_{2}O maser disk.
The kinematical data were analyzed with the classical method that is based on the rotation curves, and with a new method developed by us that is based on spectroastrometry.
The classical method indicates that the gas disk has inclination and position angles consistent with those of a largescale galactic disk. The disk rotates in a gravitational potential resulting from an extended stellar mass distribution and a spatially unresolved dynamical mass of (1.7 ± 0.2) × 10^{7} M_{⊙}, concentrated within r < 7 pc, corresponding to the seeinglimited resolution of the observations. The estimates of inclination, position angle, and mass are consistent with previous measurements based on SINFONI spectroscopy.
The spectroastrometric method is capable of probing the gas rotation at scales that are a factor ~3.5 smaller than those set by the spatial resolution. The dynamical mass that is spatially unresolved at the scales probed by spectroastrometry is a factor ~2 smaller, , than that recovered from the rotation curve analysis, indicating that spectroastrometry has spatially resolved the nuclear mass distribution down to 2 pc scales. This unresolved mass is still a factor ~4.5 larger than the BH mass measurement obtained with the H_{2}O maser emission, indicating that, even with spectroastrometry, it has not been possible to resolve the sphere of influence of the BH.
Based on the detailed analysis by Müller Sanchez et al. (2006), this dark mass distribution is likely composed of warm molecular gas as revealed by the H_{2} 1−0 S(1) emission at 2.12 μm. This medium has a high density, is clumpy and forming stars, and has been tentatively identified with the molecular torus required by the AGN unified model, which prevents a direct view of the central BH in Circinus. The mass distribution is similar in shape to that of the nuclear star cluster of the Milky Way. We tentatively speculate that molecular tori, forming stars at a high rate, might be the precursors of the nuclear star clusters that are common in latetype spirals.
Acknowledgments
We wish to honor the memory of our great friend and colleague David Axon. He will be greatly missed by all of us. We are grateful to Roberto Maiolino for providing us the reduced HST NICMOS images. A.G. and A.M. acknowledge financial support from the Italian National Institute for Astrophysics by INAF CRAM 1.06.09.10.
References
 Prieto, A. M., Marco, O., & Gallimore, J. 2005, MNRAS, 364, L28 [NASA ADS] [Google Scholar]
 Avni, Y. 1976, ApJ, 210, 642 [NASA ADS] [CrossRef] [Google Scholar]
 Bailey, J. 1998, MNRAS, 301, 161 [NASA ADS] [CrossRef] [Google Scholar]
 Baines, D., Oudmaijer, R. D., Mora, A., et al. 2004, MNRAS, 353, 697 [NASA ADS] [CrossRef] [Google Scholar]
 Bower, R. G., Benson, A. J., Malbon, R., et al. 2006, MNRAS, 370, 645 [NASA ADS] [CrossRef] [Google Scholar]
 Cappellari, M., & Emsellem, E. 2004, PASP, 116, 138 [NASA ADS] [CrossRef] [Google Scholar]
 Cappellari, M., Neumayer, N., Reunanen, J., et al. 2009, MNRAS, 394, 660 [NASA ADS] [CrossRef] [Google Scholar]
 Davies, R. I., Thomas, J., Genzel, R., et al. 2006, ApJ, 646, 754 [NASA ADS] [CrossRef] [Google Scholar]
 Di Matteo, T., Springel, V., & Hernquist, L. 2005, Nature, 433, 604 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Efron, B., & Tibshirani, R. J. 1994, in Introduction to the Bootstrap (Chapman & Hall/CRC) [Google Scholar]
 Fabian, A. C., & Iwasawa, K. 1999, MNRAS, 303, L34 [NASA ADS] [CrossRef] [Google Scholar]
 Ferrarese, L., & Ford, H. 2005, Space Sci. Rev., 116, 523 [NASA ADS] [CrossRef] [Google Scholar]
 Ferrarese, L., & Merritt, D. 2000, ApJ, 539, L9 [NASA ADS] [CrossRef] [Google Scholar]
 Freeman, K. C., Karlsson, B., Lynga, G., et al. 1977, A&A, 55, 445 [NASA ADS] [Google Scholar]
 Gebhardt, K., Bender, R., Bower, G., et al. 2000, ApJ, 539, L13 [NASA ADS] [CrossRef] [Google Scholar]
 Genzel, R., Eisenhauer, F., & Gillessen, S. 2010, Rev. Mod. Phys., 82, 3121 [NASA ADS] [CrossRef] [Google Scholar]
 Gnerucci, A., Marconi, A., Capetti, A., Axon, D. J., & Robinson, A. 2010, A&A, 511, A19 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Gnerucci, A., Marconi, A., Cresci, G., et al. 2011, A&A, 533, A124 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Graham, A. W. 2008a, ApJ, 680, 143 [NASA ADS] [CrossRef] [Google Scholar]
 Graham, A. W. 2008b, PASA, 25, 167 [NASA ADS] [CrossRef] [Google Scholar]
 Granato, G. L., De Zotti, G., Silva, L., Bressan, A., & Danese, L. 2004, ApJ, 600, 580 [Google Scholar]
 Greenhill, L. J., Booth, R. S., Ellingsen, S. P., et al. 2003a, ApJ, 590, 162 [NASA ADS] [CrossRef] [Google Scholar]
 Greenhill, L. J., Kondratko, P. T., Lovell, J. E. J., et al. 2003b, ApJ, 582, L11 [NASA ADS] [CrossRef] [Google Scholar]
 Hicks, E. K. S., Davies, R. I., Malkan, M. A., et al. 2009, ApJ, 696, 448 [NASA ADS] [CrossRef] [Google Scholar]
 Häring, N., & Rix, H. 2004, ApJ, 604, L89 [NASA ADS] [CrossRef] [Google Scholar]
 Kaeufl, H.U., Ballester, P., Biereichel, P., et al. 2004, in SPIE Conf. Ser. 5492, eds. A. F. M. Moorwood, & M. Iye, 1218 [Google Scholar]
 Kormendy, J., & Richstone, D. 1995, ARA&A, 33, 581 [NASA ADS] [CrossRef] [Google Scholar]
 Krajnović, D., Sharp, R., & Thatte, N. 2007, MNRAS, 374, 385 [NASA ADS] [CrossRef] [Google Scholar]
 Krajnović, D., McDermid, R. M., Cappellari, M., & Davies, R. L. 2009, MNRAS, 399, 1839 [NASA ADS] [CrossRef] [Google Scholar]
 Macchetto, F., Marconi, A., Axon, D. J., et al. 1997, ApJ, 489, 579 [NASA ADS] [CrossRef] [Google Scholar]
 Maiolino, R., AlonsoHerrero, A., Anders, S., et al. 2000, ApJ, 531, 219 [NASA ADS] [CrossRef] [Google Scholar]
 Marconi, A., & Hunt, L. K. 2003, ApJ, 589, L21 [NASA ADS] [CrossRef] [Google Scholar]
 Marconi, A., Moorwood, A. F. M., Origlia, L., & Oliva, E. 1994, The Messenger, 78, 20 [NASA ADS] [Google Scholar]
 Marconi, A., Axon, D. J., Capetti, A., et al. 2003, ApJ, 586, 868 [NASA ADS] [CrossRef] [Google Scholar]
 Marconi, A., Risaliti, G., Gilli, R., et al. 2004, MNRAS, 351, 169 [NASA ADS] [CrossRef] [Google Scholar]
 Marconi, A., Pastorini, G., Pacini, F., et al. 2006, A&A, 448, 921 [Google Scholar]
 Menci, N. 2006, Mem. Soc. Astron. Italiana, 77, 670 [NASA ADS] [Google Scholar]
 Müller Sanchez, F., Davies, R. I., Eisenhauer, F., et al. 2006, A&A, 454, 481 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 MüllerSanchez, F., Prieto, M. A., Hicks, E. K. S., et al. 2011, ApJ, 739, 69 [NASA ADS] [CrossRef] [Google Scholar]
 Neumayer, N., Cappellari, M., van der Werf, P., et al. 2010, The Messenger, 139, 36 [NASA ADS] [Google Scholar]
 Nowak, N., Saglia, R. P., Thomas, J., et al. 2007, MNRAS, 379, 909 [NASA ADS] [CrossRef] [Google Scholar]
 Nowak, N., Thomas, J., Erwin, P., et al. 2010, MNRAS, 403, 646 [NASA ADS] [CrossRef] [Google Scholar]
 Oliva, E., Salvati, M., Moorwood, A. F. M., & Marconi, A. 1994, A&A, 288, 457 [NASA ADS] [Google Scholar]
 Oliva, E., Marconi, A., Cimatti, A., & Alighieri, S. D. S. 1998, A&A, 329, L21 [NASA ADS] [Google Scholar]
 Porter, J. M., Oudmaijer, R. D., & Baines, D. 2004, A&A, 428, 327 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Porter, J. M., Oudmaijer, R. D., & Baines, D. 2005, in The Nature and Evolution of Disks Around Hot Stars, eds. R. Ignace, & K. G. Gayley, ASP Conf. Ser., 337, 299 [Google Scholar]
 Prieto, M. A., Meisenheimer, K., Marco, O., et al. 2004, ApJ, 614, 135 [NASA ADS] [CrossRef] [Google Scholar]
 Rusli, S. P., Thomas, J., Erwin, P., et al. 2011, MNRAS, 410, 1223 [NASA ADS] [CrossRef] [Google Scholar]
 Sani, E., Marconi, A., Hunt, L. K., & Risaliti, G. 2010, MNRAS, 413, 1479 [Google Scholar]
 Silk, J., & Rees, M. J. 1998, A&A, 331, L1 [NASA ADS] [Google Scholar]
 Soltan, A. 1982, MNRAS, 200, 115 [NASA ADS] [CrossRef] [Google Scholar]
 Tadhunter, C., Marconi, A., Axon, D., et al. 2003, MNRAS, 342, 861 [NASA ADS] [CrossRef] [Google Scholar]
 Takami, M., Bailey, J., & Chrysostomou, A. 2003, A&A, 401, 655 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 van der Marel, R. P., & van den Bosch, F. C. 1998, AJ, 116, 2220 [NASA ADS] [CrossRef] [Google Scholar]
 Whelan, E. T., Ray, T. P., Bacciotti, F., et al. 2005, in Protostars and Planets V, 8073 [Google Scholar]
 Yu, Q., & Tremaine, S. 2002, MNRAS, 335, 965 [NASA ADS] [CrossRef] [Google Scholar]
All Tables
All Figures
Fig. 1 Continuumsubtracted detector 3 CRIRES spectrum (slit PA1) extracted at the position of the continuum peak. Solid red line: fit to Brγ using a GaussHermite function. 

In the text 
Fig. 2 Rotation curves for the CRIRES Brγ spectra. Left panel: slit PA1. Central panel: slit PA2. Right panel: slit PA3. The solid red lines represent the curves expected from the model. 

In the text 
Fig. 3 Surface brightness profiles of the Brγ line along the slits (black lines). The red lines represent the surface brightness of the underlying continuum. 

In the text 
Fig. 4 Upper panel: fit of the NICMOS F222m light profile. The black continuous line represents the bestfit model. The dotdashed line represents the profile of the compact component ( FWHM size) and the dashed line the extended component. The compact component is detected and identified with hot dust emission in NACO observations by Prieto et al. (2004). The spatial extension of the compact component is similar to that of the NICMOS PSF and therefore the first Airy ring is still visible. Lower panel: model residuals. 

In the text 
Fig. 5 χ^{2} vs. i curve for the determination of best value and confidence interval of the disk inclination. The dotted lines represents the 1, 2, and 3σ confidence levels. 

In the text 
Fig. 6 Confidence regions in the M_{UDM}M/L plane for the rotation curve model fits. The isocontours indicate the 95%, 90%, and 68% (the inner one) confidence levels. The dotted line marks the M_{UDM}M/L values corresponding to the minimum χ^{2} fit. The open circles indicate the grid of values used in the M_{UDM}M/L plane. 

In the text 
Fig. 7 Position velocity diagram of the continuumsubtracted Brγ spectrum at PA1. Upper panel: observed spectrum. Bottom panel: synthetic reconstruction. The horizontal dotted line overplotted on each panel represents the continuum peak position. The isophotes denote the same values in both panels. 

In the text 
Fig. 8 Spectroastrometric curves of the Brγ line at the three slit position angles. Left panel: PA1. Central panel: PA2. Right panel: PA3. The dashed vertical lines in each panel represent the limits of the HV range. Wavelengths are converted into velocity using as reference (zero velocity) the rest frame Brγ wavelength (2.1661 μm). 

In the text 
Fig. 9 2D spectroastrometric map for the Brγ line. The red point marks the inferred position of the pointlike mass. The red solid line represents the line of nodes of the disk obtained from a linear fit to the HV points, as described in the text. The dotted red lines represent the 1σ uncertainties on the position angle of line of nodes. The origin of the map is the position on the sky plane of the PA1 slit center (which corresponds to the continuum peak position). 

In the text 
Fig. 10 Results of the fit to the spectroastrometric Brγ data. The left panel shows the rotation curve projected along the line of nodes, S_{ch} vs. V_{ch}. The right panel shows the r = S_{ch} − S_{0} vs. V = V_{ch} − V_{sys} rotation curve. The solid red lines represent the curves expected from the model. The dotted line in right panel represents the rotation curve due to the star component of the gravitational potential. 

In the text 
Fig. 11 Dynamical mass measurements in the nuclear region of the Circinus galaxy. Measurements are marked by filled circles of different colors and are identified in the legend. The red filled circle represents the CRIRES spectroastrometry mass measurement obtained assuming a disk with i = 61° with respect to the line of sight, same as the largescale measurements; the open red circle represents the spectroastrometry mass measurement obtained assuming an edgeon disk, same as the maser disk. The region shaded by gray dotted lines is characterized by r < 20 mas and is the region probed by the H_{2}O maser rotation curve, where the dynamical mass is mostly unresolved and belongs to the BH. The enclosed mass within this region must be dominated by the BH, since no evidence for extended mass is seen in the maser rotation curve. The gray stripe represents the radial total mass distribution of the bestfit model for the CRIRES rotation curves (taking into account errors on M_{UDM} and M/L). The orange line represents the total mass distribution, which is a combination of BH mass, nuclear (4 pc size) and extended mass distribution, with the mass distribution derived by Müller Sanchez et al. (2006). The nuclear mass distribution corresponds to what we measure as M_{UDM}. The green line is similar to the orange line but the nuclear mass distribution now has a size of 2 pc. The dashed green line is the contribution of BH mass and nuclear mass distribution, while the dotted line represents the BH mass and the extended mass distribution. The continuous black line represents the radial mass distribution of the nuclear star cluster at the center of the Milky Way (Genzel et al. 2010) combined with the BH mass (Greenhill et al. 2003a) and rescaled to match the measurements at ~10 pc scale. 

In the text 
Current usage metrics show cumulative count of Article Views (fulltext article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 4896 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.