EDP Sciences logo
Subscriber Authentication Point
Search
Menu
Home All issues Volume 518 (July-August 2010) A&A, 518 (2010) L53 Full HTML
Issue
A&A
Volume 518, July-August 2010
Herschel: the first science highlights
Article Number L53
Number of page(s) 5
Section Letters
DOI https://doi.org/10.1051/0004-6361/201014555
Published online 16 July 2010
A&A 518, L53 (2010)

Herschel: the first science highlights

LETTER TO THE EDITOR

The Herschel Virgo Cluster Survey

VI. The far-infrared view of M 87[*]

M. Baes1 - M. Clemens2 - E. M. Xilouris3 - J. Fritz1 - W. D. Cotton4 - J. I. Davies5 - G. J. Bendo6 - S. Bianchi7 - L. Cortese5 - I. De Looze1 - M. Pohlen5 - J. Verstappen1 - H. Böhringer8 - D. J. Bomans9 - A. Boselli10 - E. Corbelli7 - A. Dariush5 - S. di Serego Alighieri7 - D. Fadda11 - D. A. Garcia-Appadoo12 - G. Gavazzi13 - C. Giovanardi7 - M. Grossi14 - T. M. Hughes5 - L. K. Hunt7 - A. P. Jones15 - S. Madden16 - D. Pierini8 - S. Sabatini17 - M. W. L. Smith5 - C. Vlahakis18 - S. Zibetti19

1 - Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, 9000 Gent, Belgium
2 - INAF-Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 35122 Padova, Italy
3 - National Observatory of Athens, I. Metaxa and Vas. Pavlou, P. Penteli, 15236 Athens, Greece
4 - National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA, 22903-2475, USA
5 - Department of Physics and Astronomy, Cardiff University, The Parade, Cardiff, CF24 3AA, UK
6 - Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, UK
7 - INAF-Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, 50125 Firenze, Italy
8 - Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, Postfach 1312, 85741, Garching, Germany
9 - Astronomical Institute, Ruhr-University Bochum, Universitaetsstr. 150, 44780 Bochum, Germany
10 - Laboratoire d'Astrophysique de Marseille, UMR 6110 CNRS, 38 rue F. Joliot-Curie, 13388 Marseille, France
11 - NASA Herschel Science Center, California Institute of Technology, MS 100-22, Pasadena, CA 91125, USA
12 - ESO, Alonso de Cordova 3107, Vitacura, Santiago, Chile
13 - Università di Milano-Bicocca, piazza della Scienza 3, 20100, Milano, Italy
14 - CAAUL, Observatório Astronómico de Lisboa, Universidade de Lisboa, Tapada da Ajuda, 1349-018, Lisboa, Portugal
15 - Institut d'Astrophysique Spatiale (IAS), Batiment 121, Universite Paris-Sud 11 and CNRS, 91405 Orsay, France
16 - Laboratoire AIM, CEA/DSM - CNRS - Université Paris Diderot, Irfu/Service d'Astrophysique, 91191 Gif-sur-Yvette, France
17 - INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica, via Fosso del Cavaliere 100, 00133, Roma, Italy
18 - Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
19 - Max-Planck-Institut für Astronomie, Koenigstuhl 17, 69117 Heidelberg, Germany

Received 30 March 2010 / Accepted 2 May 2010

Abstract
The origin of the far-infrared emission from the nearby radio galaxy M 87 remains a matter of debate. Some studies find evidence of a far-infrared excess due to thermal dust emission, whereas others propose that the far-infrared emission can be explained by synchrotron emission without the need for an additional dust emission component. We present Herschel PACS and SPIRE observations of M 87, taken as part of the science demonstration phase observations of the Herschel Virgo Cluster Survey. We compare these data with a synchrotron model based on mid-infrared, far-infrared, submm and radio data from the literature to investigate the origin of the far-infrared emission. Both the integrated SED and the Herschel surface brightness maps are adequately explained by synchrotron emission. At odds with previous claims, we find no evidence of a diffuse dust component in M 87, which is not unexpected in the harsh X-ray environment of this radio galaxy sitting at the core of the Virgo cluster.

Key words: galaxies: individual: M 87 - radiation mechanisms: thermal - radiation mechanisms: non-thermal - infrared: galaxies

1 Introduction

At a distance of 16.7 Mpc (Mei et al. 2007), M 87 is the dominant galaxy of the Virgo cluster. It is one of the nearest radio galaxies and was the first extragalactic X-ray source to be identified. Because of its proximity, many interesting astrophysical phenomena can be studied in more detail in M 87 than in other comparable objects (see e.g. Röser & Meisenheimer 1999, for an overview). Among its many remarkable features is the several billion solar mass supermassive black hole at its centre (Gebhardt & Thomas 2009; Macchetto et al. 1997) and the prominent jet extending from the nucleus, visible throughout the electromagnetic spectrum. The central regions of M 87, in particular the structure of the jet, have been studied and compared intensively at radio, optical, and X-ray wavelengths (e.g. Kovalev et al. 2007; Perlman et al. 2001; Perlman & Wilson 2005; Sparks et al. 2004; Meisenheimer et al. 1996; Werner et al. 2010; Biretta et al. 1991; Böhringer et al. 2001; Simionescu et al. 2008).

Compared to the available information at these wavelengths, our knowledge of M 87 at far-infrared (FIR) wavelengths is rather poor. A controversial issue is the origin of the FIR emission in M 87, i.e., the question of whether the FIR emission is caused entirely by synchrotron emission or whether there is an additional contribution from dust associated with either the global interstellar medium or a nuclear dust component. This question is partly driven by the observation of faint dust features in deep optical images (Ferrarese et al. 2006; Sparks et al. 1993). Several papers on the FIR emission of M 87 arrive at different conclusions. Perlman et al. (2007) present ground-based Subaru and Spitzer IRS spectra of the M 87 nucleus and find evidence of an excess at wavelengths longer than 25 $\mu $m, which they attribute to thermal emission from cool dust at a characteristic temperature of some 55 K. This claim is countered by Buson et al. (2009), who present a higher signal-to-noise IRS spectrum of the nucleus. After careful subtraction of a stellar emission template from the mid-infrared spectrum, these authors conclude that the nuclear spectrum can be fully accounted for by optically thin synchrotron emission and that there is little room for dust emission. On a larger scale, Xilouris et al. (2004) present ISOCAM imaging of M 87 and argue that the mid-infrared flux can be attributed to a single synchrotron emission component. Shi et al. (2007) present Spitzer IRAC and MIPS imaging of M 87 and find a slight excess in the FIR over a power-law interpolation. They attribute this excess emission to dust emission from the host galaxy. Finally, Tan et al. (2008) observed 1.3 mm continuum emission from the nucleus and jet of M 87 and found that the measured fluxes are generally consistent with synchrotron emission, although they could not rule out a possible nuclear contribution from thermal dust emission.

The recently launched Herschel Space Observatory (Pilbratt et al. 2010) offers the possibility to study M 87 at FIR wavelengths in more detail than has been possible to date. The PACS (Poglitsch et al. 2010) and SPIRE (Griffin et al. 2010) instruments combined can produce images over the wavelength range between 70 and 500 $\mu $m with unprecedented sensitivity and superior resolution. In this Letter, we present PACS and SPIRE imaging of M 87 at 100, 160, 250, 350, and 500 $\mu $m, taken as part of the science demonstration phase (SDP) observations of the Herschel Virgo Cluster Survey (HeViCS[*]). We combine these observations with mid-infrared, FIR, submm, and radio data from the literature to investigate the level and the origin of the FIR emission in M 87. In Sect. 2, we present the observations and data reduction, Sect. 3 describes the analysis of the data and in Sect. 4 we present our conclusions.

\begin{figure} \par\includegraphics[width=8.8cm,clip]{14555fg1.eps} \vspace{-2mm} \end{figure} Figure 1:

The Herschel view of the central regions of M 87. The bottom right image is a VLA 20 cm image from the FIRST survey. The 20 cm radio contours have been overlaid on the Herschel images. The field of view of all images is $160\hbox {$^{\prime \prime }$ }\times 90\hbox {$^{\prime \prime }$ }$, beam sizes are indicated in the bottom right corner.

Open with DEXTER

2 Observations and data reduction

We observed M 87 on 29 November 2009 with PACS and SPIRE as part of the HeViCS SDP observations. The HeViCS SDP field covers a $4\times4$ deg2 field at the centre of the Virgo cluster, roughly centred on M 87. It was scanned with a 60 $^{\prime \prime }$/s scanning speed in nomimal and orthogonal directions. Data were gathered simultaneously in the green and red PACS bands (100 and 160 $\mu $m) and the three SPIRE bands (250, 350, and 500 $\mu $m). The PACS and SPIRE data were reduced using HIPE, with reduction scripts based on the standard reduction pipelines. For more details of the HeViCS SDP data reduction, we refer to Davies et al. (2010). Figure 1 shows the Herschel images at the five PACS and SPIRE bands of the central $160\hbox {$^{\prime \prime }$ }\times 90\hbox {$^{\prime \prime }$ }$ regions of M 87, which is clearly detected in all five bands.

\begin{figure} \par\includegraphics[width=8.5cm,clip]{14555fg2.eps} \vspace*{-2mm} \end{figure} Figure 2:

Top: the global SED of M 87 from mid-infrared to radio wavelengths. When no error bars are seen, they are smaller than the symbol size. The solid line in the plot is the best-fit power law of the ISOCAM, IRAS, MIPS, SCUBA, GBT, WMAP, and VLA data; the dotted line has only been fitted to the SCUBA, GBT, WMAP, and VLA data. Bottom: residual between data and the best-fit synchrotron model in the infrared-submm wavelength range. The cyan line is a modified black-body model with T=23 K and $M_{\rm{d}}=7\times10^4~M_\odot$ (see text).

Open with DEXTER

Table 1:   Integrated fluxes for M 87 in the infrared-submm wavelength region between 15 and 1000 $\mu $m.

\begin{figure} \par\includegraphics[width=14.5cm,clip]{14555fg3.eps} \end{figure} Figure 3:

A comparison between the data and a synchrotron model. The three images on the top row show the observed Spitzer image of M 87 at 24 $\mu $m and VLA images at 2 cm and 100 cm, all convolved to the same resolution (8.5 $^{\prime \prime }$ FWHM, 2 $^{\prime \prime }$ pixels). In each pixel, a synchrotron emission was fit to the Spitzer, GBT, and VLA data accross the wavelength range between 24 $\mu $m and 100 cm. The solid lines in the images show the region where the data are reliable at all wavelengths: outside this region, not all images could be used. The bottom row images show the synchrotron model images corresponding to the images on the top row. The two rightmost images show the slope of the synchrotron fit and the curvature of the fit, both at 6 cm.

Open with DEXTER

3 Analysis

The most straightforward, first-order approach to investigating the origin of the FIR emission in M 87 is to study its global spectral energy distribution (SED). Table 1 lists the Herschel fluxes of M 87, together with ISOCAM, IRAS, MIPS, and SCUBA data gathered from the literature (Golombek et al. 1988; Xilouris et al. 2004; Haas et al. 2004; Shi et al. 2007). The top panel in Fig. 2 shows the SED in the infrared-submm-radio region between 15 $\mu $m and 100 cm. Apart from the infrared-submm fluxes from Table 1, this plot shows GBT MUSTANG and VLA radio continuum fluxes from Cotton et al. (2009) and the most recent 5-year WMAP fluxes from Wright et al. (2009). The solid line is the best-fit power law for the ISOCAM, IRAS, MIPS, SCUBA, GBT, WMAP, and VLA data and has a slope $\alpha=-0.76$; the dotted line fits only the SCUBA, GBT, WMAP, and VLA data and has a slope $\alpha=-0.74$.

The bottom panel in Fig. 2 shows the residual from the best-fit power law in the infrared-submm wavelength region; it is clear that the integrated Herschel fluxes are in full agreement with synchrotron radiation. The cyan line in this figure is a modified black-body fitted with T=23 K and $M_{\rm{d}}=7\times10^4~M_\odot$. This temperature is the mean dust equilibrium temperature in the interstellar radiation field of M 87, determined using the SKIRT radiative transfer code (Baes et al. 2003,2005) and based on the photometry from Kormendy et al. (2009). The dust mass was adjusted to fit the upper limits of the residuals. It is clear that the SED of M 87 is incompatible with dust masses higher than $10^5~M_\odot$.

Although indicative, the analysis of the integrated SED does not definitely identify the origin of the FIR emission in M 87. Approximating the global SED as a single power-law synchrotron model is indeeed an oversimplification of the complicated structure of M 87. The bottom-right panel of Fig. 1 shows a high-resolution 20 cm image from the VLA FIRST survey (White et al. 1997; Becker et al. 1995), its contours being superimposed on the Herschel images. This 20 cm image identifies three distinct regions of significant synchrotron emission: the nucleus, the jet and associated lobes in the NW region, and the SE lobes. It is well-known that these different components have different spectral indices (e.g., Cotton et al. 2009; Shi et al. 2007) - detailed studies have shown that even within the jet, the spectral index can vary significantly (Perlman et al. 2001; Biretta et al. 1991; Meisenheimer et al. 1996). A spatially resolved analysis of the different regions of M 87 is therefore a more powerful tool for investigating the origin of the FIR emission. Unfortunately, a full spatially resolved analysis of M 87 using all Herschel bands is impractical. On the one hand, the PACS PSF is smeared significantly due to the rapid scan speed and the PACS images have a limited signal-to-noise ratio (hereafter S/N). The SPIRE images on the other hand have higher S/N, but the beam size is relatively large for a full spatially resolved analysis of the different components. The M 87 nucleus, jet, and associated NW lobes are discernible in the three SPIRE bands, but the identification of faint emission in the SE lobes is difficult, particularly in the 500 $\mu $m band. We therefore concentrated our efforts on the 250 $\mu $m image, which provides the optimal compromise between S/N and spatial resolution.

Our analysis consisted of constructing a synchrotron model for the central regions of M 87, based on the available ancillary images with sufficient field-of-view, resolution, and surface brightness sensitivity. We use the new 90 GHz radio continuum maps taken with the MUSTANG bolometer array presented by Cotton et al. (2009). These data have a resolution of 8 $.\!\!^{\prime\prime}$5 FWHM, hence closely match our Herschel data. The same authors also present archival VLA data at 15, 8.2, 4.9, 1.6, and 0.3 GHz of similar resolution, which were also used in our analysis. An image at 23 GHz was also available in the VLA archive, but it was not used in our analysis because it may be insensitive to extended structure because of a lack of short interferometer baselines. Finally, a Spitzer MIPS image at 24 $\mu $m was extracted from the archive and reduced using the MIPS Data Analysis Tools (Gordon et al. 2005), as described in Young et al. (2009). As noted by Shi et al. (2007), a faint extended halo is visible in the 24 $\mu $m image, which is probably caused by stellar emission and/or circumstellar dust. Because of the complexity of the image, we did not attempt to subtract this faint emission from the map; since the flux density in the central regions of M 87 is strongly dominated by non-thermal emission from the nucleus, jet, and lobes, we are confident that this decision does not affect our results.

As a first step, we convolved the available images to the same resolution (8 $.\!\!^{\prime\prime}$5 FWHM), shifted them to the same astrometry (2 $^{\prime \prime }$ pixel scale), and converted them to similar surface brightness units (MJy sr-1). The result is a data cube with seven points in the wavelength dimension covering an impressive wavelength range of nearly 5 orders of magnitude. Following the same strategy as Cotton et al. (2009), we fitted a second-order polynomial synchrotron model to each pixel of this data cube. The fits were performed with the MPFIT robust non-linear least squares curve fitting library in IDL (Markwardt 2009).

Figure 3 shows a comparison between the data and the resulting synchrotron models at 24 $\mu $m, 2 cm, and 100 cm. The solid white line in these figures borders the spatial region where reliable surface brightnesses were available at all seven wavelengths. Outside this region, spectral fits were still made, but typically used fewer data points, e.g., because one of the radio images contained negative flux at the corresponding wavelengths. By inspecting the images on the top row, it is obvious that the synchrotron emission is not homogeneous in the different regions: the short wavelength radiation is dominated by the central source, whereas the jet and lobes dominate at the longer wavelengths. Comparing the top row panels with the corresponding bottom row panels, however, one can clearly see that, in spite of this different structure, our simple synchrotron model can reproduce the observed images very well over the entire wavelength range. The right-hand panels of Fig. 3 show the slope and the curvature of the synchrotron model at the reference wavelength of 6 cm. The slope varies from -0.4 in the nuclear region to -0.8, and the curvature is modest ranging from slightly positive in the very faint regions to about -0.06 in nucleus, jet, and lobes. These values are consistent with the values found by Cotton et al. (2009), who limited their fits to the radio regime between 3.3 mm and 100 cm.

For the next step in our analysis, we used our synchrotron model to predict the emission of M 87 at 250 $\mu $m. The left panel of Fig. 4 shows the synchrotron model prediction at 250 $\mu $m at the model resolution. By far the brightest peak of the model is located at the position of the nucleus; the jet is clearly visible as a second bright component, whereas the SE lobe is visible as an extended, low surface brightness region with a peak surface brightness that is almost five times fainter than the nucleus (23 MJy sr-1 versus 110 MJy sr-1). When we convolve this synchrotron model image with the SPIRE 250 $\mu $m beam and rebin it to match the observed SPIRE image astrometry, the three different components corresponding to nucleus, jet, and SE lobes merge into a single extended structure with one elongated peak 4 $^{\prime \prime }$ to the west of the nucleus. Comparing the central and right panels of Fig. 4, we see that the synchrotron model is capable of explaining the observed SPIRE 250 $\mu $m image satisfactorily.

\begin{figure} \par\includegraphics[width=0.485\textwidth]{14555fg4.eps} % \end{figure} Figure 4:

A comparison between the synchrotron model image and the observed image at 250 $\mu $m. The left panel shows the synchrotron image at the model resolution (8 $.\!\!^{\prime\prime}$5 FWHM, 2 $^{\prime \prime }$ pixels), the central panel shows the same model convolved to the SPIRE 250 $\mu $m beam and pixel size (18 $.\!\!^{\prime\prime}$1 FWHM, 6 $^{\prime \prime }$ pixels). The right panel shows the observed SPIRE 250 $\mu $m image. In all panels, the green lines are the contours of the synchrotron model at the model resolution.

Open with DEXTER

4 Conclusion

For both the integrated SED and the SPIRE 250 $\mu $m map, we have found that synchrotron emission is an adequate explanation of the FIR emission. We do not detect a FIR excess that cannot be explained by the synchrotron model. In particular, we have no reason to invoke the presence of smooth dust emission associated with the galaxy interstellar medium, as advocated by Shi et al. (2007). For a dust temperature of 23 K, which is the expected equilibrium temperature in the interstellar radiation field of M 87, we find an upper limit to the dust mass of $7\times10^4~M_\odot$.Our result agrees with the analysis of the nuclear emission by Buson et al. (2009). Clemens et al. (2010) discuss the lifetimes of interstellar dust grains in elliptical galaxies in the Virgo cluster based on Herschel observations and find an upper limit to the amorphous silicate grain survival time of less than 46 million years. Given that M 87 is a luminous X-ray source, the absence of a substantial dust component is not a surprise. A low dust content is also in agreement with the non-detection of cool molecular gas (Tan et al. 2008; Salomé & Combes 2008) and the non-detection of significant intrinsic absorption in the X-ray spectra of M 87 (Böhringer et al. 2002). Our conclusion is that, seen from the FIR point of view, M 87 is a passive object with a central radio source emitting synchrotron emission, without a substantial diffuse dust component.

Acknowledgements
The National Radio Astronomy Observatory (NRAO) is operated by Associated Universities Inc, under cooperative agreement with the National Science Foundation.

References

  1. Baes, M., Davies, J. I., Dejonghe, H., et al. 2003, MNRAS, 343, 1081 Baes, M., Dejonghe, H., & Davies, J. I. 2005, The Spectral Energy Distributions of Gas-Rich Galaxies: Confronting Models with Data, AIP Conf. Proc., 761, 27 [NASA ADS] [CrossRef] [Google Scholar]
  2. Becker, R. H., White, R. L., & Helfand, D. J. 1995, ApJ, 450, 559 [NASA ADS] [CrossRef] [Google Scholar]
  3. Biretta, J. A., Stern, C. P., & Harris, D. E. 1991, AJ, 101, 1632 [NASA ADS] [CrossRef] [Google Scholar]
  4. Böhringer, H., Belsole, E., Kennea, J., et al. 2001, A&A, 365, L181 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  5. Böhringer, H., Matsushita, K., Churazov, E., Ikebe, Y., & Chen, Y. 2002, A&A, 382, 804 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  6. Buson, L., Bressan, A., Panuzzo, P., et al. 2009, ApJ, 705, 356 [NASA ADS] [CrossRef] [Google Scholar]
  7. Clemens, M. S., et al. 2010, A&A, 518, L50 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  8. Cotton, W. D., Mason, B. S., Dicker, S. R., et al. 2009, ApJ, 701, 1872 [NASA ADS] [CrossRef] [Google Scholar]
  9. Davies, J. I., et al. 2010, A&A, 518, L48 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  10. Ferrarese, L., Côté, P., Jordán, A., et al. 2006, ApJS, 164, 334 [NASA ADS] [CrossRef] [Google Scholar]
  11. Gebhardt, K., & Thomas, J. 2009, ApJ, 700, 1690 [NASA ADS] [CrossRef] [Google Scholar]
  12. Golombek, D., Miley, G. K., & Neugebauer, G. 1988, AJ, 95, 26 [NASA ADS] [CrossRef] [Google Scholar]
  13. Gordon, K. D., Rieke, G. H., Engelbracht, C. W., et al. 2005, PASP, 117, 503 [NASA ADS] [CrossRef] [Google Scholar]
  14. Griffin, M. J., et al. 2010, A&A, 518, L3 [Google Scholar]
  15. Haas, M., Müller, S. A. H., Bertoldi, F., et al. 2004, A&A, 424, 531 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  16. Kormendy, J., Fisher, D. B., Cornell, M. E., & Bender, R. 2009, ApJS, 182, 216 [NASA ADS] [CrossRef] [Google Scholar]
  17. Kovalev, Y. Y., Lister, M. L., Homan, D. C., & Kellermann, K. I. 2007, ApJ, 668, L27 [NASA ADS] [CrossRef] [Google Scholar]
  18. Macchetto, F., Marconi, A., Axon, D. J., et al. 1997, ApJ, 489, 579 [NASA ADS] [CrossRef] [Google Scholar]
  19. Markwardt, C. B. 2009, ASP Conf. Ser., 411, 251 [Google Scholar]
  20. Marshall, H. L., Miller, B. P., Davis, D. S., et al. 2002, ApJ, 564, 683 [NASA ADS] [CrossRef] [Google Scholar]
  21. Mei, S., Blakeslee, J. P., Côté, P., et al. 2007, ApJ, 655, 144 [NASA ADS] [CrossRef] [Google Scholar]
  22. Meisenheimer, K., Roeser, H.-J., & Schloetelburg, M. 1996, A&A, 307, 61 [NASA ADS] [Google Scholar]
  23. Owen, F. N., Eilek, J. A., & Kassim, N. E. 2000, ApJ, 543, 611 [NASA ADS] [CrossRef] [Google Scholar]
  24. Perlman, E. S., & Wilson, A. S. 2005, ApJ, 627, 140 [NASA ADS] [CrossRef] [Google Scholar]
  25. Perlman, E. S., Biretta, J. A., Sparks, W. B., Macchetto, F. D., & Leahy, J. P. 2001, ApJ, 551, 206 [NASA ADS] [CrossRef] [Google Scholar]
  26. Perlman, E. S., Mason, R. E., Packham, C., et al. 2007, ApJ, 663, 808 [NASA ADS] [CrossRef] [Google Scholar]
  27. Pilbratt, G. L., et al. 2010, A&A, 518, L1 [CrossRef] [EDP Sciences] [Google Scholar]
  28. Poglitsch, A., et al. 2010, A&A, 518, L2 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  29. Röser, H.-J., & Meisenheimer, K. 1999, The Radio Galaxy Messier, 87, 530 [Google Scholar]
  30. Salomé, P., & Combes, F. 2008, A&A, 489, 101 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  31. Shi, Y., Rieke, G. H., Hines, D. C., Gordon, K. D., & Egami, E. 2007, ApJ, 655, 781 [NASA ADS] [CrossRef] [Google Scholar]
  32. Simionescu, A., Werner, N., Finoguenov, A., Böhringer, H., & Brüggen, M. 2008, A&A, 482, 97 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  33. Sparks, W. B., Ford, H. C., & Kinney, A. L. 1993, ApJ, 413, 531 [NASA ADS] [CrossRef] [Google Scholar]
  34. Sparks, W. B., Donahue, M., Jordán, A., Ferrarese, L., & Côté, P. 2004, ApJ, 607, 294 [NASA ADS] [CrossRef] [Google Scholar]
  35. Swinyard, B. M., Ade, P., Baluteau, J.-P., et al. 2010, A&A, 518, L4 [Google Scholar]
  36. Tan, J. C., Beuther, H., Walter, F., & Blackman, E. G. 2008, ApJ, 689, 775 [NASA ADS] [CrossRef] [Google Scholar]
  37. Xilouris, E. M., Madden, S. C., Galliano, F., Vigroux, L., & Sauvage, M. 2004, A&A, 416, 41 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  38. Werner, N., Simionescu, A., Million, E. T., et al. 2010, MNRAS, accepted [arXiv:1003.5334] [Google Scholar]
  39. White, R. L., Becker, R. H., Helfand, D. J., & Gregg, M. D. 1997, ApJ, 475, 479 [NASA ADS] [CrossRef] [Google Scholar]
  40. Wright, E. L., Chen, X., Odegard, N., et al. 2009, ApJS, 180, 283 [NASA ADS] [CrossRef] [Google Scholar]
  41. Young, L. M., Bendo, G. J., & Lucero, D. M. 2009, AJ, 137, 3053 [NASA ADS] [CrossRef] [Google Scholar]

Footnotes

... M 87[*]
Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
... (HeViCS[*]
More details on HeViCS can be found on http://www.hevics.org

All Tables

Table 1:   Integrated fluxes for M 87 in the infrared-submm wavelength region between 15 and 1000 $\mu $m.

All Figures

  \begin{figure} \par\includegraphics[width=8.8cm,clip]{14555fg1.eps} \vspace{-2mm} \end{figure} Figure 1:

The Herschel view of the central regions of M 87. The bottom right image is a VLA 20 cm image from the FIRST survey. The 20 cm radio contours have been overlaid on the Herschel images. The field of view of all images is $160\hbox {$^{\prime \prime }$ }\times 90\hbox {$^{\prime \prime }$ }$, beam sizes are indicated in the bottom right corner.

Open with DEXTER
In the text

  \begin{figure} \par\includegraphics[width=8.5cm,clip]{14555fg2.eps} \vspace*{-2mm} \end{figure} Figure 2:

Top: the global SED of M 87 from mid-infrared to radio wavelengths. When no error bars are seen, they are smaller than the symbol size. The solid line in the plot is the best-fit power law of the ISOCAM, IRAS, MIPS, SCUBA, GBT, WMAP, and VLA data; the dotted line has only been fitted to the SCUBA, GBT, WMAP, and VLA data. Bottom: residual between data and the best-fit synchrotron model in the infrared-submm wavelength range. The cyan line is a modified black-body model with T=23 K and $M_{\rm{d}}=7\times10^4~M_\odot$ (see text).

Open with DEXTER
In the text

  \begin{figure} \par\includegraphics[width=14.5cm,clip]{14555fg3.eps} \end{figure} Figure 3:

A comparison between the data and a synchrotron model. The three images on the top row show the observed Spitzer image of M 87 at 24 $\mu $m and VLA images at 2 cm and 100 cm, all convolved to the same resolution (8.5 $^{\prime \prime }$ FWHM, 2 $^{\prime \prime }$ pixels). In each pixel, a synchrotron emission was fit to the Spitzer, GBT, and VLA data accross the wavelength range between 24 $\mu $m and 100 cm. The solid lines in the images show the region where the data are reliable at all wavelengths: outside this region, not all images could be used. The bottom row images show the synchrotron model images corresponding to the images on the top row. The two rightmost images show the slope of the synchrotron fit and the curvature of the fit, both at 6 cm.

Open with DEXTER
In the text

  \begin{figure} \par\includegraphics[width=0.485\textwidth]{14555fg4.eps} % \end{figure} Figure 4:

A comparison between the synchrotron model image and the observed image at 250 $\mu $m. The left panel shows the synchrotron image at the model resolution (8 $.\!\!^{\prime\prime}$5 FWHM, 2 $^{\prime \prime }$ pixels), the central panel shows the same model convolved to the SPIRE 250 $\mu $m beam and pixel size (18 $.\!\!^{\prime\prime}$1 FWHM, 6 $^{\prime \prime }$ pixels). The right panel shows the observed SPIRE 250 $\mu $m image. In all panels, the green lines are the contours of the synchrotron model at the model resolution.

Open with DEXTER
In the text

Copyright ESO 2010

Current usage metrics show cumulative count of Article Views (full-text 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 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.