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A&A 518, L45 (2010) DOI: 10.1051/0004-6361/201014530
c ESO 2010

Astronomy & Astrophysics
Special feature
Letter to the Editor

Herschel: the first science highlights

The dust morphology of the elliptical Galaxy M 86 with SPIRE
H. L. Gomez1 , M. Baes2 , L. Cortese1 ,M.W.L.Smith1 ,A.Boselli3 , L. Ciesla3 ,G.J. Bendo4 ,M.Pohlen1 , S. di Serego Alighieri5 ,R.Auld1 ,M.J. Barlow6 , J. J. Bock7 , M. Bradford7 , V. Buat3 , N. Castro-Rodriguez8 , P. Chanial9 ,S.Charlot10 , D.L.Clements4 ,A.Cooray11 , D. Cormier9 , J. I. Davies1 , E. Dwek12 , S. Eales1 , D. Elbaz9 , M. Galametz9 , F. Galliano9 ,W.K.Gear1 , J. Glenn13 , M. Griffin1 , S. Hony9 , K. G. Isaak14 ,L.R.Levenson7 , N. Lu7 , S. Madden9 , B. O'Halloran3 , K. Okumura9 ,S.Oliver15 , M. J. Page16 ,P.Panuzzo9 , A. Papageorgiou1 , T. J. Parkin17 , I. Perez-Fournon8 ,N.Rangwala13 ,E.E.Rigby18 , H. Roussel10 ,A.Rykala1 , N. Sacchi19 ,M. Sauvage9 , M. R. P. Schirm17 ,B.Schulz20 , L. Spinoglio19 , S. Srinivasan10 , J.A.Stevens21 , M. Symeonidis16 , M. Trichas4 , M. Vaccari22 ,L.Vigroux10 ,C.D.Wilson17 ,H.Wozniak23 ,G.S.Wright24 , and W. W. Zeilinger25
(Affiliations are available in the online edition) Received 29 March 2010 / Accepted 25 April 2010
ABSTRACT

We present Herschel-SPIRE observations at 250-500 m of the giant elliptical galaxy M 86 and examine the distribution of the resolved cold emission and its relation with other galactic tracers. The SPIRE images reveal three dust components: emission from the central region; a lane extending north-south; and a bright emission feature 10 kpc to the south-east. We estimate that 106 M of dust is spatially coincident atomic and ionized hydrogen, originating from stripped material from the nearby spiral NGC 4438 due to recent tidal interactions with M 86. gas-to-dust ratio of the cold gas component ranges from 20-80. We discuss the different heating mechanisms for the dust features.
Key words. galaxies: ellipticals and lenticular, cD ­ galaxies: individual: M 86 ­ submillimeter: ISM ­ dust, extinction

dust dust wi t h The

1. Introduction
Studies of cold dust in elliptical galaxies has been limited to date by the lack of high-resolution, long wavelength spectral coverage. In particular, the origin of far-infrared (FIR) emission in these systems is still a controversial issue, with evidence of dusty disks favouring a stellar origin (e.g. Knapp et al. 1989) and other systems originating from mergers with dust-rich galaxies (Leeuw et al. 2008). The unprecedented resolution and sensitivity of the recently launched Herschel Space Observatory (Pilbratt et al. 2010) allows us to address long-standing issues such as the origin and quantity of dust in ellipticals. One of the most well-known IR-bright ellipticals is the giant Virgo cluster member, M 86, at a distance of 17 Mpc (Mei et al. 2007). Two dust features were detected with IRAS, one coincident with the galaxy and another to the north-west, thought to be coincident with an X-ray plume of gas (Knapp et al. 1989; White et al. 1991) and originally attributed to dust stripped from M 86 due to its motion through the cluster. Higher resolution data from ISO revealed two dust peaks within M 86 suggesting a massive dust complex (Stickel et al. 2003, hereafter S03). They proposed a tidal origin, also supported by absorption features attributed to dust stripped from the nearby dwarf galaxy, VCC 882 (Elmegreen et al. 2000). The discovery of atomic gas offset from the centre of M 86 and decoupled from its stellar disk supports the tidal scenario (Li & van Gorkom 2001). More recently,
Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.

Kenney et al. (2008, hereafter K08) detected strong H features extending from the nearby spiral NGC 4438 at 23 away, to within 1 of the nucleus of M 86. The distribution and velocity of the ionized gas provides clear evidence for tidal interaction between these two giants (K08, Fig. 1 Cortese et al. 2010). In this scenario, we are observing debris from the spiral left in the wake of the collision with M 86 with 109 M of cold gas removed from NGC 4438 (K08). The stripped material is then heated by the hot interstellar medium (ISM) of M 86 or shock fronts from the interaction. Although tidal stripping from NGC 4438 is supported by the atomic and ionized gas distribution, the origin of the dust responsible for the FIR emission and its heating mechanism is unclear. Here we present submm observations of M 86 with Herschel-SPIRE (Griffinet al. 2010). Companion observations of NGC 4438, are presented in Cortese et al. (2010).

2. Observations and data reduction
M 86 was observed with SPIRE at 250, 350 and 500 m during Herschel's science demonstration phase as part of the Herschel Reference Survey (Boselli et al. 2010a). Eight pairs of crosslinked observations were taken in scan-map mode with scanning rate 30 /s. The data were processed following the detailed description given in Pohlen et al. (2010) and Bendo et al. (2010a). Calibration methods and accuracies are outlined in Swinyard et al. (2010). The measured 1 noise level is 5, 6 and 7 mJy beam-1 at 250, 350 and 500 m with beam size 18, 25 and 37 ; the noise is dominated by background source confusion. Page 1 of 5

Article published by EDP Sciences


A&A 518, L45 (2010)

Fig. 1. Left: R-band image of M 86 region with H (red) and X-ray (green) contours. Right: three-colour image at 250, 350 and 500 m, smoothed to 500 m beam (as indicated by dashed circle in upper right of the figure). The ellipse indicates the optical halo of M 86 (8.9 â 5.6 ).

3. Results
The three-colour SPIRE image is shown in Fig. 1 with dust features labeled (following the terminology of S03) along with an optical image of the same region with X-ray and H contours. In the SPIRE image, there are a number of unresolved sources, and at least five extended features. Careful comparison of large scale FUV and IRAS maps of this region show that the cirrus emission is extremely low ruling out a Galactic origin. In Fig. 2, we focus on the central 13 â 8 region and compare with structures seen at other wavelengths. Towards the south, M 86-S is coincident with a number of clustered 24 m sources. In the north-west, the bright source M 86-NW (originally associated with M 86's X-ray plume) has no optical or UV counterpart and peaks at < 100 m. The bright feature M 86-FIR5 is coincident with an optical galaxy (VPC 463) and, like M 86-FIR4, has a similar flux ratio to M 86-NW. Extending north from M 86, a faint (2-3) filament-like submm structure appears to be coincident with blueshifted H emission (Fig. 2) attributed to ionized debris from the incoming trajectory of the NGC 4438 collision (Trinchieri & di Serego Alighieri 1991; Finoguenov et al. 2004; K08). However, this submm filament is also coincident with a number of distant 24 m sources. We therefore suggest that this feature along with M 86-S, M 86-NW, M 86-FIR5 and M 86FIR4 originate from background sources unrelated to M 86. The submm morphology within the inner 2 of M 86 is surprisingly complex and differs from the smooth distributions seen in the 24 m, UV and optical images. We see four distinct features in the SPIRE maps labeled as M 86-N, M 86-off, M 86-SE and "lane" (Fig. 1). M 86-N is a bright unresolved source which is included in the photometry due to its coincidence with a H knot in this region1. The feature M 86-SE (7.7 â 2.3 kpc) is the brightest feature within the optical halo and is offset from the centre by 1.9 (10 kpc). To the immediate north of this feature extends the bright "lane" structure. These features are not seen in the Spitzer 24 or 70 m data (although the latter exhibits severe striping effects) but are detected with ISO at 90, 135 and 180 m
We note that M 86-N has similar features to other point sources in the crowded field and could be a background object. It contributes 15% of the flux measured in the aperture for M 86-off. Page 2 of 5
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and Spitzer 160 m(Fig. 2). Although there are four 24 m point sources coincident with the M 86-SE structure, these are likely to be background sources since corresponding features are not seen in the same position in H nor are they coincident with the peaks in the submm emission. These four features (Fig. 2) are spatially coincident with peaks in the redshifted ionized gas (M 86-SE: -120 km s-1, M 86-off: -200-350 km s-1) extending from NGC 4438 (K08) and with atomic Hi (Li & van Gorkom 2001). The submm and Hi peak in M 86-SE is coincident with an H "hole", but this is likely due to the lower resolution of the former. M 86-SE is also contained within an X-ray boundary tracing the X-ray halo (Finoguenov et al. 2004; Randall et al. 2008). The strong spatial correlation between the cool atomic gas, cold dust, ionised gas and hot X-ray boundary shown in Fig. 2 seems to suggest that the dust originates from gas stripped from NGC 4438 and is immersed in the X-Ray halo of M 86. At first glance, it appears that the "lane" feature and M 86-SE are coincident with dusty filaments seen in absorption (A and B in Fig. 2; Elmegreen et al. 2000). Careful comparison with the SPIRE images show that their B feature is 1.3 south of M 86-SE, and filament A is offset by 0.4 . Faint submm emission is seen at the southern tip of A and the atomic gas encompasses feature B. We are not able to resolve A (at only 6 across in the optical), but surprisingly we do not detect significant emission associated with B. This could be a result of the absorption features arising from foreground dust lanes with low column density, or the dust is simply too cold to be detected with Herschel.
3.1. Dust mass and heating within the optical halo

We performed aperture photometry on the IR and submm images from ISO, Spitzer and SPIRE. The datasets were wcs-aligned, and smoothed to the 160 m beam using the appropriate kernels (Bendo et al. 2010b) and assuming Gaussian beam profiles for SPIRE. Fluxes were measured using two elliptical apertures (Fig. 2) with semi-major, semi-minor axes and position angles of 1.4 â 1.0 , 127.5 (encompassing M 86-SE) and 1.0 â 1.6 ,31.5 (encompassing M 86-off and M 86-N) respectively. We used an empirical 160 m PSF to determine the aperture correction (Young et al. 2009). The spectral energy distributions (SEDs) of


H. L. Gomez et al.: Herschel-SPIRE observations of M 86

Fig. 2. Multiwavelength comparison of M 86. Top: UV (GALEX) and optical (SDSS) with absorption features A & B. Middle: Spitzer 24-160 m and SPIRE 250-500 m. White ellipses indicate photometry apertures. Bottom: gas emission shown in negative greyscale. Hi with white contours 10 + 25 mJy beam-1 (courtesy J. van Gorkom). H (courtesy J. Kenney) and X-ray (ROSAT). 250 m shown by red contours 9 + 6 mJy beam-1 .

M 86-off and M 86-SE are shown in Fig. 3 (see also Boselli et al. 2010b). Blackbody functions modified with a -2 emissivity law are plotted for comparison with temperatures 15 K and 44 K. Assuming a mass-absorption coefficient, 500 = 0.1kg-1 m2 (Draine 2003), we can estimate a rough dust mass from the total 500 m flux, S 500 assuming Md = S D2 / B(, T ) where D is the distance. The total dust mass within the inner 2 of M 86 ranges from 2-5 â 106 M for temperatures, T d = 15-20 K. Comparing the dust masses with the atomic gas mass, we estimate a range of gas-to-dust ratios of g/d 20-80 depending on the temperature. Non-detection of CO gas within M 86 rules out a significant molecular component with <106.8 M (Braine et al. 1997). The ionized gas could contribute a further 107 M , but this is difficult to estimate without knowing the gas densities (K08). These ratios are higher than expected in elliptical galaxies (e.g. Fich & Hodge 1993) and similar to the lower range of values estimated for the dust feature extending out from NGC 4438 (Cortese et al. 2010).

It is interesting to ask what is responsible for heating the dust and creating the submm emission seen here. Possible mechanisms include AGN, the interstellar radiation field (ISRF), tidal heating and/or the hot X-ray halo. Following Thomas et al. (2002), the luminosity Lh required to heat a cloud of dust with grain size a,total mass Md , temperature T d and Planck-averaged absorption coefficient Q(a, T d ) ,is given by Eq. (1): Lh = 4a md
2 4 Q(a, T d) T d Md .

(1)

For a < 0.1 m at 20 K, we require Lh < 109 L . M 86 is radio quiet and we can rule out significant heating from the AGN. Although the dust is not spatially coincident with the optical/UV, the ISRF could still be responsible for heating the dust with Lh comparable to the B-Band luminosity (Mei et al. 2007). To investigate this, we used a radiative transfer implementation of the Monte Carlo code skirt (Baes & Dejonghe 2002), which
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A&A 518, L45 (2010)

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100

10 1000 Flux (mJy)

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from the centre, towards the southeast. The unprecedented resolution of SPIRE has revealed, for the first time, a strong spatial correlation between the cold dust (106 M , g/d of 20-80) and the warm ionized gas in M 86. This result strongly favours a scenario whereby the dust in M 86 originates from material stripped from the nearby spiral NGC 4438. We investigate the different heating mechanisms responsible for the dust emission detected by Herschel. Intriguingly, although we cannot rule out the stellar radiation field of M 86, the strong correlation between submm and H emission suggests the cold dust is heated by the same mechanisms responsible for ionizing the gas stripped from NGC 4438. If so, tidal heating is likely to be responsible for the dust emission. Further modeling is required to provide a definite answer on the origin of the submm features revealed by SPIRE in M 86.
Acknowledgements. We thank Jeff Kenney & Jacqueline van Gorkom for providing electronic versions of their data. The images were produced with APLpy, thanks to Edward Gomez & Eli Bressart. We thank the referee for their constructive comments. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, OAMP (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCLMSSL, UKATC, Univ. Sussex (UK); and Caltech/JPL, IPAC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Observatory (Sweden); STFC (UK); and NASA (USA).

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Fig. 3. The SEDs for top: M 86-SE and bottom: M 86-off. Solid lines are modified blackbody functions with cold temperature 15 K and 44 K. Spitzer fluxes are blue triangles, ISO (stars) and SPIRE (circles). IRAS data (green triangles) are measured in a single aperture of radius 136 .

models the absorption, scattering and thermal emission of circumstellar discs and dusty galaxies. M 86 was represented by a flattened Sersic model based on parameters from the literature (Caon et al. 1993; Graham & Colless 1997; Gavazzi et al. 2005) and we used the global SED from Boselli et al. (2010b) for the intrinsic model. During the Monte Carlo simulation, the mean intensity of the radiation field is calculated from UV-MIR wavelengths at every position in the galaxy. From this mean intensity, the equilibrium dust temperature, T eq of each species of dust grains is calculated using energy balance. We predict that T eq for silicate (graphite) grains at a distance of 1.9 from the nucleus is 13 (19) K; even though the submm peaks do not correlate with optical/UV emission, the ISRF of M 86 is sufficient to produce the submm emission detected here. The thermal energy provided by M 86's hot, X-ray emitting ISM could also provide a significant heating contribution by collisionally heating the dust, with grains of a < 0.1 m reaching T eq < 18 K (e.g. Dwek 1987). The tidally-heated component as traced by H also cannot be ruled out as it provides comparable energy to M 86's thermal reservoir over the last 100 Myr (109 L , K08). Thus, the ISRF, X-ray halo and tidal heating could all be contributing to heating the dust and it is difficult to separate these processes using the UV-submm SED only. However, the high resolution images presented here suggest that submm emission only originates from regions where we detect atomic and ionised gas. Submm emission is not detected from regions with just atomic Hi and X-ray emission, suggesting that the X-ray halo alone is not responsible for heating the dust. The spatial distribution of these tracers therefore favours a scenario in which the submm emission originates from dust mixed with stripped atomic material and is heated by the tidal interaction. In summary, we present submm images of M 86 which reveal a complex dust morphology with emission detected 10 kpc

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School of Physics & Astronomy, Cardiff University, The Parade, Cardiff, CF24 3AA, UK e-mail: haley.gomez@astro.cf.ac.uk Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, 9000 Gent, Belgium Astrophysics Group, Imperial College, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, UK Laboratoire d'Astrophysique de Marseille, UMR6110 CNRS, 38 rue F. Joliot-Curie, 13388 Marseille, France INAF-Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy Dept. of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK Jet Propulsion Laboratory, Pasadena, CA 91109, California Institute of Technology, Pasadena, CA 91125, USA Instituto de AstrofÌsica de Canarias (IAC) and Departamento de AstrofÌsica, Universidad de La Laguna (ULL), La Laguna, Tenerife, Spain CEA, Laboratoire AIM, Irfu/SAp, Orme des Merisiers, 91191 Gif-sur-Yvette, France Institut d'Astrophysique de Paris, UMR7095 CNRS, 98 bis Boulevard Arago, 75014 Paris, France Dept. of Physics & Astronomy, University of California, Irvine, CA 92697, USA Observational Cosmology Lab, Code 665, NASA Goddard Space Flight Center Greenbelt, MD 20771, USA

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Department of Astrophysical and Planetary Sciences, CASA CB389, University of Colorado, Boulder, CO 80309, US ESA Astrophysics Missions Division, ESTEC, PO Box 299, 2200 AG Noordwijk, The Netherlands Astronomy Centre, Department of Physics and Astronomy, University of Sussex, UK Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT, UK Dept. of Physics & Astronomy, McMaster University, Hamilton, Ontario, L8S 4M1, Canada School of Physics & Astronomy, University of Nottingham, University Park, Nottingham NG7 2RD, UK Istituto di Fisica dello Spazio Interplanetario, INAF, via del Fosso del Cavaliere 100, 00133 Roma, Italy Infrared Processing and Analysis Center, California Institute of Technology, 770 South Wilson Av, Pasadena, CA 91125, USA Centre for Astrophysics Research, Science and Technology Research Centre, University of Hertfordshire, Herts AL10 9AB, UK University of Padova, Department of Astronomy, Vicolo Osservatorio 3, 35122 Padova, Italy Observatoire Astronomique de Strasbourg, UMR 7550 UniversitÈ de Strasbourg - CNRS, 11, rue de l'UniversitÈ, 67000 Strasbourg, France UK Astronomy Technology Center, Royal Observatory Edinburgh, Edinburgh, EH9 3HJ, UK Institut fÝr Astronomie, UniversitÄt Wien, TÝrkenschanzstr. 17, 1180 Wien, Austria

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