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A&A
Volume 518, July-August 2010
Herschel: the first science highlights
Article Number L60
Number of page(s) 5
Section Letters
DOI https://doi.org/10.1051/0004-6361/201014592
Published online 16 July 2010
A&A 518, L60 (2010)

Herschel: the first science highlights

LETTER TO THE EDITOR

Far-infrared line imaging of the starburst ring in NGC 1097 with the Herschel/PACS spectrometer[*]

P. Beirão1 - L. Armus1 - P. N. Appleton2 - J.-D. T. Smith3 - K. V. Croxall3 - E. J. Murphy1 - D. A. Dale4 - G. Helou2 - R. C. Kennicutt5 - D. Calzetti6 - A. D. Bolatto7 - B. R. Brandl8 - A. F. Crocker6 - B. T. Draine9 - G. Dumas10 - C. W. Engelbracht11 - A. Gil de Paz12 - K. D. Gordon13 - B. Groves8 - C.-N. Hao14 - J. L. Hinz11 - L. K. Hunt15 - B. D. Johnson5 - J. Koda16 - O. Krause10 - A. K. Leroy17,[*] - S. E. Meidt10 - J. Richer18 - H.-W. Rix10 - N. Rahman19 - H. Roussel21 - K. M. Sandstrom10 - M. Sauvage22 - E. Schinnerer10 - R. A. Skibba11 - S. Srinivasan21 - F. Walter10 - B. E. Warren19 - C. D. Wilson20 - M. G. Wolfire7 - S. Zibetti10

1 - Spitzer Science Center, California Institute of Technology, MC 314-6, Pasadena, CA 91125, USA
2 - NASA Herschel Science Center, IPAC, California Institute of Technology, Pasadena, CA 91125, USA
3 - Department of Physics and Astronomy, Mail Drop 111, University of Toledo, 2801 West Bancroft Street, Toledo, OH 43606, USA
4 - Department of Physics & Astronomy, University of Wyoming, Laramie, WY 82071, USA
5 - Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
6 - Department of Astronomy, University of Massachusetts, Amherst, MA 01003, USA
7 - Department of Astronomy, University of Maryland, College Park, MD 20742, USA
8 - Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
9 - Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA
10 - Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
11 - Steward Observatory, University of Arizona, Tucson, AZ 85721, USA
12 - Departamento de Astrofisica, Facultad de Ciencias Fisicas, Universidad Complutense Madrid, Ciudad Universitaria, Madrid, 28040, Spain
13 - Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
14 - Tianjin Astrophysics Center, Tianjin Normal University, Tianjin 300387, PR China
15 - INAF - Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
16 - Department of Physics and Astronomy, SUNY Stony Brook, Stony Brook, NY 11794-3800, USA
17 - National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA
18 - Astrophysics Group, Cavendish Laboratory, J. J. Thomson Avenue, Cambridge CB3 0HE; Kavli Institute for Cosmology, c/o Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
19 - ICRAR, M468, University of Western Australia, 35 Stirling Hwy, Crawley, WA, 6009, Australia
20 - Deptartment of Physics & Astronomy, McMaster University, Hamilton, Ontario L8S 4M1, Canada
21 - Institut d'Astrophysique de Paris, UMR7095 CNRS Université Pierre & Marie Curie, 98 bis boulevard Arago, 75014 Paris, France
22 - CEA/DSM/DAPNIA/Service d'Astrophysique, UMR AIM, CE Saclay, 91191 Gif-sur-Yvette Cedex, France

Received 30 March 2010 / Accepted 3 May 2010

Abstract
NGC 1097 is a nearby SBb galaxy with a Seyfert nucleus and a bright starburst ring. We study the physical properties of the interstellar medium (ISM) in the ring using spatially resolved far-infrared spectral maps of the circumnuclear starburst ring of NGC 1097, obtained with the PACS spectrometer on board the Herschel Space Observatory. In particular, we map the important ISM cooling and diagnostic emission lines of [OI] 63 $\mu $m, [OIII] 88 $\mu $m, [NII] 122 $\mu $m, [CII] 158 $\mu $m and [NII] 205 $\mu $m. We observe that in the [OI] 63 $\mu $m, [OIII] 88 $\mu $m, and [NII] 122 $\mu $m line maps, the emission is enhanced in clumps along the NE part of the ring. We observe evidence of rapid rotation in the circumnuclear ring, with a rotation velocity of $\sim$220 km s-1 (inclination uncorrected) measured in all lines. The [OI] 63 $\mu $m/[CII] 158 $\mu $m ratio varies smoothly throughout the central region, and is enhanced on the northeastern part of the ring, which may indicate a stronger radiation field. This enhancement coincides with peaks in the [OI] 63 $\mu $m and [OIII] 88 $\mu $m maps. Variations of the [NII] 122 $\mu $m/[NII] 205 $\mu $m ratio correspond to a range in the ionized gas density between 150 and 400 cm-3.

Key words: photon-dominated region - infrared: galaxies - galaxies: Seyfert - galaxies: starburst - techniques: imaging spectroscopy - galaxies: individual: NGC 1097

1 Introduction

NGC 1097 is a Seyfert 1 galaxy with a bright starburst ring with a diameter of 2 kpc and a strong large-scale bar (Hsieh et al. 2008; Kohno et al. 2003; Gerin et al. 1988) with a length of 15 kpc. Optical and near-infrared images reveal dust lanes that run along the primary large-scale (15 kpc) bar and curve into the ring, which is formed by two very tight spiral arms, and a second bar inside the ring (Quillen et al. 1995; Prieto et al. 2005). This bar may be responsible for driving gas into the nucleus, possibly fueling the central super-massive black hole (Davies et al. 2009; Prieto et al. 2005; Fathi et al. 2006), and may also have triggered the formation of a compact star cluster seen near the nucleus. NGC 1097 provides an excellent opportunity to study the physical conditions of the interstellar medium (ISM) in a nearby galaxy with both a starburst and an active nucleus.

The nucleus and the star-forming ring are prominent in CO and HCN line emission (Kohno et al. 2003). Near-infrared spectroscopy (Kotilainen et al. 2000; Reunanen et al. 2002) reveals emission from both ro-vibrational H2 and H-recombination lines at the nucleus, the star-forming ring, and the region in between. Optical long-slit spectroscopy (Storchi-Bergmann et al. 1996) shows strong ionized gas emission from both the nucleus and the ring, along with faint line emission from the inner region, exhibiting a LINER-type spectrum.

With Herschel/PACS (Poglitsch et al. 2010) we are now able to target the most important cooling lines of the warm ISM on physical scales much smaller than ever before possible in external galaxies. The KINGFISH project (Key Insights on Nearby Galaxies: a Far-Infrared Survey with Herschel - PI: R. C. Kennicutt) is an open-time Herschel key program which aims to measure the heating and cooling of the gaseous and dust components of the ISM in a sample of 61 nearby galaxies with the PACS and SPIRE instruments. The far infrared spectral range covered by PACS includes several of the most important cooling lines of the atomic gas, notably [CII] 158 $\mu $m, [OI] 63 $\mu $m, [OIII] 88 $\mu $m, [NII] 122 $\mu $m, and [NII] 205 $\mu $m. NGC 1097 is one of the KINGFISH targets selected for the Herschel science demonstration program (SDP) (for PACS imaging of NGC 1097 see Sandstrom et al. 2010 and for SPIRE observations see Engelbracht et al. 2010).

In this letter, we present far-infrared spectral line maps of the circumnuclear starburst ring and the large-scale bar of NGC 1097, obtained with the PACS spectrometer on board the ESA Herschel Space Observatory (Pilbratt et al. 2010). The maps presented in this letter are the first PACS spectral maps from the KINGFISH program. Throughout this paper we assume a distance to NGC 1097 of 19.1 Mpc (Willick et al. 1997), which gives a projected scale of $1\hbox{$^{\prime\prime}$ }=92$ pc.

2 Observations and data reduction

\begin{figure} \par\includegraphics[width=8cm,clip]{14592fg1} \end{figure} Figure 1:

Composite of [CII] 158 $\mu $m emission maps in the center (yellow contours) and extranuclear positions (red contours), overlaid on a Spitzer/MIPS 24 $\mu $m image of NGC 1097 (in grayscale). The extranuclear maps are a combination of wavelength-switching data (North) and chop-nod data (South). The contour levels in units of 10-7 W/m2/sr are: 0.35, 0.70, 1.4, 2.8, 4.2, and 5.95 for the nucleus, 0.092, 0.184, 0.276, 0.368, 0.460, and 0.570 for the southern extranuclear region, and 0.051, 0.102, 0.153, 0.204, and 0.238 for the northern extranuclear region.

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NGC 1097 was observed with the $5\times5$ pixel integral field unit (IFU) of the PACS Spectrometer in both chop-nod (CN) and wavelength switching (WS) modes as part of a series of science demonstration phase tests. The field of view of the IFU is $47\hbox{$^{\prime\prime}$ }\times47\hbox{$^{\prime\prime}$ }$ with $9\hbox{$.\!\!^{\prime\prime}$ }4$ pixels (Poglitsch et al. 2010). The diffraction limited FWHM beam size of PACS is $5\hbox{$.\!\!^{\prime\prime}$ }2$ at $60{-}85~\mu$m and $12\hbox{$^{\prime\prime}$ }$ at $130{-}210~\mu$m. The spectral resolution of PACS is 180 km s-1 for [OI] 63 $\mu $m, 120 km s-1 for [OIII] 88 $\mu $m, 290 km s-1 for [NII] 122 $\mu $m, 240 km s-1 for [CII] 158 $\mu $m, and 150 km s-1 for [NII] 205 $\mu $m. CN observations were carried out between January 4 and January 22, 2010, with an observing time of 19.4 h, with 17.7 h on-source. WS observations were carried out between January 4 and January 22, 2010, and the observing time was 6.6 h, of which 3.6 h are on-source. Five different regions were observed: the nucleus, two extranuclear positions at the outer ends of the bar, and one strip at each side of the nucleus, following the minor axis of the galaxy. CN observations were obtained in a $2 \times 2$ raster in the nucleus for all five target lines (with a step size of $9\hbox{$.\!\!^{\prime\prime}$ }4$), in a single short strip along the minor axis ([OI] 63 $\mu $m, [NII] 122 $\mu $m, and [CII] 158 $\mu $m), and in a single extranuclear position to the south ([OI] 63 $\mu $m, [OIII] 88 $\mu $m, [NII] 122 $\mu $m, and [CII] 158 $\mu $m). Each map covers an area of $4.5 \times 4.5$ kpc2. In the basic CN mode, the telescope chops between two regions of sky $6\hbox{$^\prime$ }$ apart, with the target placed alternately in one or the other beam. WS observations were obtained for the same lines in a $2 \times 2$ raster in the nucleus, two short strips along the minor axis on each side of the nucleus, and in two extranuclear positions to the north and south of the nucleus. Line fluxes obtained from WS data in the same regions were in all cases comparable within the flux uncertainties to CN results, and the KINGFISH survey will utilize WS for the remainder of the sample. Here we focus on the CN observations, which have the best signal to noise ratios.

The spectra were reduced using HIPE (Herschel interactive processing environment), special development version 3.0 CIB 1134. The pipelines remove detector artifacts, obvious cosmic ray signatures and apply ground-based flat-field corrections. Dark-current subtraction was done for the WS case. Additional band-dependent scale factors were applied to the post-processed extracted fluxes to adjust the ground-based absolute calibration to in-flight observations of calibrators[*]. The uncertainty in the line fluxes is dominated by the absolute flux calibration. The flux calibration uncertainties are on the order of 30%, and pixel-to-pixel relative calibration uncertainties are on the order of 10%.

3 Results

\begin{figure} \par\includegraphics[width=8.5cm,clip]{14592fg2} \end{figure} Figure 2:

Spectral maps of the lines observed with PACS at the nuclear position, and an image of the ring at 70 $\mu $m with PACS. The maps represent the integrated flux over ${-}500 < v _{\rm sys} < 500$ km s-1, with $v_{\rm sys} = 1271$ km s-1. North is up and East is to the left. In all cases the size of the image is $51\hbox {$^{\prime \prime }$ }\times 51\hbox {$^{\prime \prime }$ }$. The cross marks the location of the radio position of the nucleus.

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In Fig. 1 we present an overlay of the [CII] 158 $\mu $m maps of the nuclear and extranuclear regions of NGC 1097 on a 24 $\mu $m image taken with the Multiband Imaging Photometer for Spitzer (MIPS) (Rieke et al. 2004). The 24 $\mu $m emission is well traced by the [CII] 158 $\mu $m emission in all the regions where [CII] 158 $\mu $m emission is observed. As there are no CN observations of the northern extranuclear region, we show a WS map, which clearly follows the detailed structure evident in the 24 $\mu $m image. The signal-to-noise ratio in the minor axis strips is very low, and these data are not shown in Fig. 1.

In Fig. 2 we present continuum-subtracted maps of the center of NGC 1097, for the [CII] 158 $\mu $m, [OI] 63 $\mu $m, [OIII] 88 $\mu $m, [NII] 122 $\mu $m, and [NII] 205 $\mu $m emission lines. For comparison, we also show a PACS 70 $\mu $m continuum image (see Sandstrom et al. 2010). The [OI] 63 $\mu $m, [OIII] 88 $\mu $m, and [NII] 122 $\mu $m maps are the most similar. There is a partial clumpy ring-like structure, with peaks NW, N and E of the nucleus in the [OI] 63 $\mu $m and [OIII] 88 $\mu $m maps, whereas the N clump is absent in the [NII] 122 $\mu $m map. The peaks observed in the [CII] 158 $\mu $m coincide with the clumps observed in the [NII] 122 $\mu $m map, but the overall distribution is much smoother. Only the N and NW peaks have a counterpart in the PACS 70 $\mu $m image. The [NII] 205 $\mu $m looks strikingly different than the other maps. It has a peak NE of the nucleus but lacks the NW and E hotspots present in the other maps. The lack of a resolved ring in the [CII] 158 $\mu $m and [NII] 205 $\mu $m may be partially due to the large beam at these wavelengths. A careful measurement of the spectrometer PSF on 10 $\hbox{$^{\prime\prime}$ }$ scales will be required in order to further separate real physical components in a system as small as the NGC 1097 ring.

\begin{figure} \par\includegraphics[width=8cm,clip]{14592fg3} \end{figure} Figure 3:

Integrated spectra of the nucleus and ring. The system velocity $v_{\rm sys} = 1271$ km s-1 is set as the zero-point, marked by the dashed-dotted line. The dashed line is the spectrum of the [CII] emission in wavelength-switching mode.

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To extract integrated spectra from the line maps, we selected a circular region of $23\hbox{$.\!\!^{\prime\prime}$ }8$ in radius centered on the nucleus which includes the ring, but avoids the noisy edges of the map. The continuum subtracted velocity profiles for each line are shown in Fig. 3. In all cases, zero velocity was defined as $v_{\rm sys} = 1271$ km s-1. An overplot of the [CII] 158 $\mu $m velocity profile made from the WS data is also shown for comparison, which has a peak flux of $\sim$90% of the CN peak, within the flux uncertainty. The smooth appearance of the [CII] 158 $\mu $m and the [NII] 122 $\mu $m line profiles is due to the worse spectral resolution at these wavelengths. The small difference is attributed to transients in the CN data which are not present in the WS data. The most notable characteristic of these profiles is that they are all double-peaked, which is expected for a rotating ring. In Fig. 4 we show the velocity map of [OI] 63 $\mu $m. The velocity spans a range of $\pm$220 km s-1, being redshifted to the SE, and blueshifted to the NW. The [OI] velocity field is consistent with circular rotation also seen in ionized (H$\alpha$, Fathi et al. 2006) and molecular gas (CO (2-1), Hsieh et al. 2008). In Table 1 we present the integrated line fluxes for the nucleus and extranuclear positions.

\begin{figure} \par\includegraphics[width=8cm,clip]{14592fg4}\vspace*{-1mm}\vspace*{-1.8mm} \end{figure} Figure 4:

Velocity field of the [OI] line in the center of NGC 1097. The contours represent approaching (blue) and receding (red) emission relative to the systemic velocity, $v_{\rm sys} = 1271$ km s-1.

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Table 1:   Integrated line fluxes1 (10-15 Wm-2).


4 Diagnosing the ionized and neutral gas properties

With the line maps we can study spatial variations in the properties of the warm atomic gas. Fine structure line ratios trace the intensity of the incident radiation field G0 on the neutral gas and the electron gas density ne, respectively (e.g., Kaufman et al. 1999). In Fig. 5 we show maps of the [OI] 63 $\mu $m/[CII] 158 $\mu $m and the [NII] 122 $\mu $m/[NII] 205 $\mu $m line ratios, overlaid with the contours of the PACS 70 $\mu $m image. Before making the ratio maps, each image was smoothed to the beam size at the longer wavelength using a Gaussian profile, while conserving flux. The [OI] 63 $\mu $m/[CII] 158 $\mu $m ratio varies smoothly with values ranging between 0.25-0.45 throughout the central region, and is enhanced on the northeast part of the ring. This enhancement partially coincides with the peaks in the [OI] 63 $\mu $m and [OIII] 88 $\mu $m line maps and the peak of the H$\alpha$ emission (Hummel et al. 1987), which indicates that the [OI] 63 $\mu $m/[CII] 158 $\mu $m ratio traces the most massive star forming knots in the ring. The values of [OI] 63 $\mu $m/[CII] 158 $\mu $m are a factor of 2 lower than for the starburst galaxy M82 (Colbert et al. 1999), but similar to the values found for most star-forming galaxies (Malhotra et al. 2001). The peak in the [OI] 63 $\mu $m/[CII] 158 $\mu $m map coincides with the N peak in the PACS 70 $\mu $m map, suggesting that at this location, a star formation rate density higher than in the rest of the ring is enhancing both dust emission and [OI] 63 $\mu $m line emission. The ratio is also enhanced on a region where the ring and the dusty spiral arms intersect, which indicate a possible shock contribution to the [OI] 63 $\mu $m flux. Models of emission lines from shocks (Hollenbach & McKee 1989) predict values of the [OI] 63 $\mu $m/[CII] 158 $\mu $m ratio of at least 10. Our measured value of $\sim$0.4 are at odds with a pure-shock interpretation of the line ratios. On the other hand, line emission from shocks cannot be ruled out because the region in the PACS beam could be a composite of both shocked gas and additional [CII] flux contributed from star formation. Models of line emission from photodissociation regions (PDRs) around O stars (e.g., Kaufman et al. 1999) show that [OI] 63 $\mu $m/[CII] 158 $\mu $m increases with the radiation field intensity G0 and neutral gas density n. However, at low densities, [OI] 63 $\mu $m/[CII] 158 $\mu $m is mostly sensitive to G0. Using Kaufman et al. (1999) models for n < 104 cm-3, we estimate G0 to lie between 60-300, and using Meijerink et al. (2007), G0 is estimated between 200-600. The higher G0 found using Meijerink et al. (2007) is likely due to their lower adopted O/C abundance ratio.

\begin{figure} \par\includegraphics[width=8cm,clip]{14592fg5a}\par\includegraphics[width=8cm,clip]{14592fg5b} \end{figure} Figure 5:

Top: map of the [OI] 63 $\mu $m/[CII] 158 $\mu $m ratio. The [OI] 63 $\mu $m map was smoothed to match the resolution at 158 $\mu $m. Bottom: map of the [NII] 122 $\mu $m/[NII] 205 $\mu $m ratio. The [NII] 122 $\mu $m map was smoothed to match the [NII] 205 $\mu $m map. Both maps are overlaid with contours from the PACS 70 $\mu $m map, after smoothing to the resolution of each map. All the ratio maps were built from line maps clipped at a 2$\sigma $ level above the noise. The cross marks the location of the nucleus.

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The [NII] 122 $\mu $m/[NII] 205 $\mu $m ratio varies between 4.0-6.0 throughout the central 40 $\hbox{$^{\prime\prime}$ }$. The values that correspond to the [NII] 122 $\mu $m peaks are 4.8 and 4.5, whereas at the [NII] 205 $\mu $m peak, the [NII] 122 $\mu $m/[NII] 205 $\mu $m ratio is 4.0. From the comparison with the 70 $\mu $m contours, we see that the highest values of the [NII] 122 $\mu $m/[NII] 205 $\mu $m ratio coincide with the ring, while the lowest are found in the inner region of the ring and also where the dust lanes meet the ring. The variations in the [NII] 122 $\mu $m/[NII] 205 $\mu $m ratio are therefore due to a variation in the ionized gas density between the ring and the inner region. Using a five level model of N+ we find that the variation of [NII] 122 $\mu $m/[NII] 205 $\mu $m ratios between the inner region and the ring corresponds to a variation of the electron density from 150 to 400 cm-3. The results are insensitive to typical gas temperatures ( $T\sim 6000{-}10~000$ K) in photoionized gas. This means that the density increases by at least a factor of 5 in the ring compared to the inner region and the region where the dust lane and the ring meet. These values are similar to the central regionof M82, in which a mean ratio value of 4.2 +1.6-1.2 was measured, corresponding to a mean electron density of 180+209-120 cm-3 across the central 50 $\hbox{$^{\prime\prime}$ }$ (Petuchowski et al. 1994). This is also consistent with the value of $\sim$220 cm-3 from the mid-infrared [SIII]18 $\mu $m/33 $\mu $m ratio over the same region (Dale et al. 2006).

The peak in the [NII] 205 $\mu $m emission line map in Fig. 2 has a line flux of $\sim$ $0.11 \times 10^{-7}$ W m-2 sr-1 and a [CII] 158 $\mu $m/[NII] 205 $\mu $m $\sim$45. For $150 < n_{{\rm e}} < 400$ cm-3 the [CII] 158 $\mu $m/[NII] 205 $\mu $m ratio in ionized gas is expected to be $\sim$3 (Oberst et al. 2006) and thus most ($\sim$90%) of the [CII] 158 $\mu $m emission we measure is coming from neutral gas. The gas heating efficiency, measured by the ([OI] + [CII])/FIR ratio, seems to stay constant in the mapped area. The $\log$ of the ratio is $\sim$-2.2 inside the ring and $\sim$-2.3 on the ring, both consistent with the values found in nearby galaxies by Malhotra et al. (2001).

In summary, we have used the PACS Spectrometer to map the [OI] 63 $\mu $m, [OIII] 88 $\mu $m, [CII] 158 $\mu $m, [NII] 122 $\mu $m and 206 $\mu $m far-infrared cooling line emission in the central 5 kpc of NGC 1097 for the first time. While the [OI] 63 $\mu $m, [OIII] 88 $\mu $m and [NII] 122 $\mu $m line maps appear qualitatively similar, the [NII] 205 $\mu $m map shows a different distribution. The [OI] 63 $\mu $m/[CII] 158 $\mu $m map shows a relative hotspot on the NE portion of the ring indicative of a stronger radiation field or a region of shocked gas. The [NII] 122 $\mu $m/[NII] 205 $\mu $m map shows a clear increase of ionized gas density in the ring, associated with massive star formation activity.

Acknowledgements
This work is based [in part] on observations made with Herschel, a European Space Agency Cornerstone Mission with significant participation by NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KUL, CSL, IMEC (Belgium); CEA, OAMP (France); MPIA (Germany); IFSI, OAP/AOT, OAA/CAISMI, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI (Italy), and CICT/MCT (Spain). Data presented in this paper were analyzed using The Herschel Interactive Processing Environment (HIPE), a joint development by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center, and the HIFI, PACS and SPIRE consortia. We would like to thank Dario Fadda and Jeff Jacobson for software support and Hanae Inami for the help on the velocity diagram.

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Footnotes

... spectrometer[*]
Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
...[*]
Hubble Fellow.
... calibrators[*]
Spectral extractions followed the prescription described in the Herschel PACS Data Reduction Guide and post-launch corrections to the ``nominal response'' followed the guidelines of Version 1.0 of the Spectroscopy and Calibration PACS release note.

All Tables

Table 1:   Integrated line fluxes1 (10-15 Wm-2).

All Figures

  \begin{figure} \par\includegraphics[width=8cm,clip]{14592fg1} \end{figure} Figure 1:

Composite of [CII] 158 $\mu $m emission maps in the center (yellow contours) and extranuclear positions (red contours), overlaid on a Spitzer/MIPS 24 $\mu $m image of NGC 1097 (in grayscale). The extranuclear maps are a combination of wavelength-switching data (North) and chop-nod data (South). The contour levels in units of 10-7 W/m2/sr are: 0.35, 0.70, 1.4, 2.8, 4.2, and 5.95 for the nucleus, 0.092, 0.184, 0.276, 0.368, 0.460, and 0.570 for the southern extranuclear region, and 0.051, 0.102, 0.153, 0.204, and 0.238 for the northern extranuclear region.

Open with DEXTER
In the text

  \begin{figure} \par\includegraphics[width=8.5cm,clip]{14592fg2} \end{figure} Figure 2:

Spectral maps of the lines observed with PACS at the nuclear position, and an image of the ring at 70 $\mu $m with PACS. The maps represent the integrated flux over ${-}500 < v _{\rm sys} < 500$ km s-1, with $v_{\rm sys} = 1271$ km s-1. North is up and East is to the left. In all cases the size of the image is $51\hbox {$^{\prime \prime }$ }\times 51\hbox {$^{\prime \prime }$ }$. The cross marks the location of the radio position of the nucleus.

Open with DEXTER
In the text

  \begin{figure} \par\includegraphics[width=8cm,clip]{14592fg3} \end{figure} Figure 3:

Integrated spectra of the nucleus and ring. The system velocity $v_{\rm sys} = 1271$ km s-1 is set as the zero-point, marked by the dashed-dotted line. The dashed line is the spectrum of the [CII] emission in wavelength-switching mode.

Open with DEXTER
In the text

  \begin{figure} \par\includegraphics[width=8cm,clip]{14592fg4}\vspace*{-1mm}\vspace*{-1.8mm} \end{figure} Figure 4:

Velocity field of the [OI] line in the center of NGC 1097. The contours represent approaching (blue) and receding (red) emission relative to the systemic velocity, $v_{\rm sys} = 1271$ km s-1.

Open with DEXTER
In the text

  \begin{figure} \par\includegraphics[width=8cm,clip]{14592fg5a}\par\includegraphics[width=8cm,clip]{14592fg5b} \end{figure} Figure 5:

Top: map of the [OI] 63 $\mu $m/[CII] 158 $\mu $m ratio. The [OI] 63 $\mu $m map was smoothed to match the resolution at 158 $\mu $m. Bottom: map of the [NII] 122 $\mu $m/[NII] 205 $\mu $m ratio. The [NII] 122 $\mu $m map was smoothed to match the [NII] 205 $\mu $m map. Both maps are overlaid with contours from the PACS 70 $\mu $m map, after smoothing to the resolution of each map. All the ratio maps were built from line maps clipped at a 2$\sigma $ level above the noise. The cross marks the location of the nucleus.

Open with DEXTER
In the text

Copyright ESO 2010

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