Free Access
Issue
A&A
Volume 573, January 2015
Article Number A116
Number of page(s) 13
Section Extragalactic astronomy
DOI https://doi.org/10.1051/0004-6361/201425105
Published online 08 January 2015

© ESO, 2015

thumbnail Fig. 1

Full spectral coverage of the ALMA Band 3 observations extracted from the nuclear position of NGC 1097 where the peak of molecular emission is observed for all species. This position corresponds to position A in Table 2 and Fig. 2.

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1. Introduction

The molecular material in galaxies is a fundamental ingredient in the fueling of the energetic phenomena in galactic nuclei. Though the mass and distribution of the molecular gas can be probed by the bright lines of carbon monoxide, deep observations of fainter molecular species have been proven as excellent tools of the physical processes affecting the molecular gas. This has been illustrated by numerous deep spectral line surveys during the last decade (see review by Martín 2011), as well as extensive work on the theoretical modeling (e.g., Meijerink et al. 2007; Bayet et al. 2008, 2011; Loenen et al. 2008; Meijerink et al. 2013; Harada et al. 2010, 2013). The molecular chemistry in the interstellar medium (ISM) provides direct information on the environmental conditions and therefore on the type of activity in the central few hundred parsecs of galaxies. Moreover, the observation of individual molecular species allow us not only to estimate the physical conditions, but also to dissect the ISM into the different heating mechanisms in play as observed within the central molecular zone of our own Galaxy (Amo-Baladrón et al. 2011; Jones et al. 2012; Martín et al. 2012).

Most of the deep and/or unbiased chemical studies in galaxies have been carried out at very low resolution (i.e.,100 pc, Wang et al. 2004; Martín et al. 2006, 2011; Aladro et al. 2011a, 2013; Davis et al. 2013; Watanabe et al. 2014) but for absorption studies toward bright continuum high-z sources where, though extremely prolific in molecular detection, no spatial information can be obtained (Muller et al. 2011, 2014). High resolution studies toward extragalactic sources have mostly focused toward the brightest nearby galaxies, as well as on the brightest species after carbon monoxide: HCN and HCO+ (NGC 253 at 3′′ resolution, Knudsen et al. (2007); M51 at 4′′, Schinnerer et al. 2010; NGC 1068 at 1′′, Krips et al. 2011; NGC 1097 at 3′′, Hsieh et al. 2012; or a sample of luminous infrarred galaxies (LIRGs) at 2′′−10′′, Imanishi et al. 2007, 2009). Imaging line surveys through interferometric observations have pushed our view of the ISM even further to show how the chemistry can provide insight into the variations of the physical processes across the central kpc of starburst (SB) galaxies (Meier & Turner 2005, 2012). However, such studies toward active galactic nucleus (AGN) galaxies have been more limited because of the lack of sensitivity (e.g., García-Burillo et al. 2010).

The full potential of extragalactic chemistry is just emerging thanks to new generation instruments, such as ALMA and the upcoming NOEMA. In fact, within the past year and while still in the early science phase, ALMA is already providing extremely high quality data on the chemistry of some of the brightest nearby prototypical galaxies, both AGNs (NGC 1068, García-Burillo et al. 2014; Takano et al. 2014; Viti et al. 2014; NGC 1097, Izumi et al. 2013) and SBs (NGC 253, Meier et al. 2014). The unprecedented capabilities of these instruments allow us to extend molecular studies to either farther or fainter objects, thus increasing the significance of chemical comparative studies, now limited to a very reduced number of sources (Aladro et al. 2014).

The prototypical nucleus in NGC 1097 hosts the first reported low-luminosity (L2−10 keV = 4.4 × 1040 ergs s-1 Terashima et al. 2002; Nemmen et al. 2006) Seyfert 1 nucleus (Storchi-Bergmann et al. 1993). The nuclear region is surrounded by a ~700 pc radius ring (Barth et al. 1995; Quillen et al. 1995) with ongoing star formation at a rate of ~5 M yr-1 (Hummel et al. 1987). The molecular material in NGC 1097 has been extensively studied at high resolution (Kohno et al. 2003; Hsieh et al. 2008, 2011, 2012). Molecular gas is distributed in a central concentration of ~350 pc that we refer to as the circumnuclear disk, directly surrounding the AGN, and the weaker 1.4 kpc diameter molecular ring, the circumnuclear star forming (SF) ring (Hsieh et al. 2008).

Though located at a similar distance (14.5 Mpc, Tully 1988) than the Seyfert 2 galaxy NGC 1068, not only the nucleus of NGC 1097 does show fainter X-ray luminosity, but it is also one order of magnitude fainter both in IR luminosity (Sanders et al. 2003) and in dense gas as traced by HCN (Hsieh et al. 2012; Krips et al. 2011). The unprecedented sensitivity of ALMA allows us to carry out multimolecule imaging studies of NGC 1097 which can be directly compared to similar studies toward the much brighter NGC 1068 (Takano et al. 2014).

In our first paper, ALMA observations of HCN and HCO+ at both J = 4−3 and 1−0 were reported by Izumi et al. (2013). In this paper we present a multimolecule imaging study that makes use of the species that were simultaneously observed with the J = 1−0 of HCN and HCO+. A companion paper will present the continuum emission in the 3 mm band, as well as a kinematic study of the ratios of the brightest species, while here we only discuss the overall integrated molecular emission. Our aim is to offer insight into the molecular abundance variations in the 300 pc region surrounding its Seyfert 1 nucleus, as compared to the star forming dominated circumnuclear ring at a distance of 600−800 pc from the center.

2. Observations

3 mm wavelength observations toward NGC 1097 were carried out as part of the ALMA Cycle 0 early science program 2011.0.00108.S (P.I. K. Kohno). Data were acquired during 2012 July 29th and October 19th with an overall on source integration time of ~72 min. The dual sideband Band 3 receivers were tuned at an LO1 frequency of 93.187 GHz. The correlator was configured in dual polarization frequency division mode (FDM) with the 4 × 1.875 GHz spectral windows covering the rest frequency ranges 85.8−89.4 GHz and 97.7−101.3 GHz (Fig. 1). The original frequency resolution of 488 kHz was degraded by 10 channels down to a velocity resolution of ~17–14.5 km s-1 across the covered frequency range.

The phase center of the observations was αJ2000 = 02h46m19.06s, δJ2000 = −30°16′29.7′′. The HPBW of the primary beam of the 12 m antennas is 72′′−61′′ at the extremes of the frequency coverage. At the distance of 14.5 Mpc, the angular to linear scale is ~70 pc/′′, therefore our observations covered the central 5−4.3 kpc at half power. The 24 and 31 antennas used on the first and second run, respectively, were configured up to distances of ~250 m from the array center, thus covering uv ranges from 4.3 to 132 (14−447 m). This configuration resulted on an average synthesized beam of ~2.2′′×1.5′′ (150 pc × 100 pc) with PA = 100°.

The quasars J1924-292 and J0334-401 were used as bandpass and phase calibrator, respectively. Absolute flux scaled was calibrated through observations toward Neptune. Data were calibrated and cleaned with CASA (McMullin et al. 2007), while images were produced with GILDAS1. A final root-mean square of ~0.5 mJy in the smoothed 4.88 MHz channels (i.e., 10 original channels) was measured in the final images.

3. Results

As shown by the spectrum in Fig. 1, extracted from the peak of molecular emission position (see below), the ~8 GHz frequency coverage of our observations allowed the detection of nine molecular species. For the identified features, Table 1 presents some basic spectral parameters extracted from JPL spectral line catalog (Pickett et al. 1998). Two non-detected transitions of HNCO (shown in brackets) are included as their limits will serve to set constraints to the excitation conditions (see Sect. 3.2).

Table 1

Spectral parameters of detected transitions.

Figure 2 presents the moment 0 maps of each of the detected species except for SO which does not stand out in the integrated maps (see discussion in Sect. 3.2). Moment 0 maps were integrated in the velocity range [900−1600] km s-1, where the molecular emission across the whole map is detected. This range was used for all species but CCH, for which the velocity range [600−1600] km s-1 (referred to the brightest hyperfine component) was integrated in order to include the two groups of hyperfine transitions. The common logarithmic color scale in Fig. 2 allows a direct comparison of the emission of the different molecular species.

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Moment 0 maps of all detected species in the velocity range [900−1600] km s-1, except for CCH where a range [600−1600] km s-1 was used to include the two groups of hyperfine components. The 1σ noise level in the integrated maps is 62 mJy km s-1 for all species, but for CCH which is 77 mJy km s-1. Logarithmic color scale is set to allow a direct comparison of the emission of the different species. Color levels are set to a minimum of 0.1 mJy km s-1 so that emission over 3σ level is seen above the black background. Positions where spectra were extracted are marked in all boxes, and labeled in the upper left box.

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3.1. Selected positions in AGN and SF ring

To study the molecular abundance variations both in the circumnuclear disk around the AGN and in the star forming ring, we have selected a sample of nine positions. Table 2 lists the relative coordinates of the selected positions referred to the phase center of the observations. Position A is selected as the brightest HCN emission position in the nuclear region of the NGC 1097 and it is offset from the phase center by (−0.9′′,0.9′′), measured at the center of the peak flux pixel in the image (with 0.45′′/pixel). This position matches the measured position of the nucleus at 6 cm (αJ2000 = 02h46m18.96s, δJ2000 = −30°16′28.9′; Hummel et al. 1987) as well as the 860 μm continuum peak (Izumi et al. 2013). The spectra extracted at this position are shown in Fig. 1.

All other positions correspond to peaks of molecular emission of the brightest species, with the selection mainly driven by the maps of the brightest species, namely HCN, C2H and CS. Figure 3 presents the individual spectra extracted from all selected positions, both in the AGN and in the SF ring.

Table 2

Coordinates and line parameters of extracted spectra.

thumbnail Fig. 3

Spectra extracted from selected positions in the AGN position (A) and on the SF ring (B-I) of NGC 1097. Frequency span has been cropped with respect to that of Fig. 1 removing the line free frequencies at the edges of both sidebands. Flux density scale has been multiplied by a factor of ×4 in the regions (defined by the vertical dashed lines) containing the fainter lines to improve their visualization. Molecular fit to the observed emission is represented by the red line. Non-detections are presented as the 3σ limit Gaussian profiles.

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3.2. Excitation and column density determination

Rather than basing our result on direct integrated intensity line ratios, we estimated the column densities of each of the molecular species to have a more accurate determination of the molecular abundances in each position.

We used the spectral line modeling tools within the MADCUBA_IJ package2 (Martín et al in prep.) to fit the molecular emission in the spectra of the selected sample positions. The main assumption of this modeling is the emission under LTE conditions. The parameters of column density, velocity and linewidth are left as free parameters. Table 2 presents the average velocity and linewidth measured in all species. See Hsieh et al. (2011) for a discussion on the kinematics and the different linewidths measured in the star forming ring cloud complexes. However, excitation temperature and the source size parameters were fixed to 8 K and 1.8′′, respectively. These assumptions are explained in the following.

The gas in both the SF ring and around the AGN have kinetic temperatures higher than our assumed excitation temperature (Tk = 30−90 K; Piñol-Ferrer et al. 2011). This is due to the fact that the molecular gas is subthermally excited. For HCN and HCO+, Izumi et al. (2013) combined the J = 1−0 and 4−3 transitions, observed with ALMA, smoothed down to the resolution of the 3−2 transition, observed with the SMA (Hsieh et al. 2012), in order to estimate the excitation conditions of the gas traced by these species. The emission can be roughly fitted in LTE by a rotational temperature of ~8 K. This result is similar in the central position A around the AGN and toward the SF ring. Though the assumption on the excitation temperature will not strongly affect the relative abundances given that most of our observed transitions have similarly low (4−10 K) energies, it might be an issue for the transition of HC3N with a significantly higher upper energy level (Table 1). However, the work by Aladro et al. (2011b) toward nearby starbursts shows that such subthermal excitation affects equally to other molecular species in their lower J transitions, to those not only at lower energies but also up to transitions with ~50 K upper energy levels. Additionally the non detection of the two higher energy transitions of HNCO listed in Table 1 and shown in Fig. 1 set a limit on the excitation temperature of this species to Tex< 20 K.

Table 3

Column densities for each species and the selected position.

thumbnail Fig. 4

Top: molecular abundances relative to HCN estimated in the sample of selected positions for all detected species. Colored histograms represent species detected while empty histograms represent upper limits to the detection. Bottom: abundances normalized to those of position A for comparison. As a reference, the three horizontal dotted lines represent equal relative abundances or a factor of two above and below those in position A.

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Regarding the source size we assume the emission to be distributed in a region approximately equal to the synthesized beam in solid angle, that is 1.8′′ or ~125 pc. A smaller emitting region would directly scale up the column density, thus increasing the effect of opacity. Our fit to the spectra results in an opacity of τ ~ 0.2 in the brightest positions (A and B) for HCN. Assuming a source size of half our assumed value would increase the opacities up to τ ≳ 1 and the derived column densities by a factor of ~5. Izumi et al. (2013) also found low opacities in the high-J transitions of HCN in the center of NGC 1097. Based on the peak line ratio of HCN and H13CN of ~15 and assuming a 12C/13C isotopic ratio of ~40 (Henkel et al. 2014) we can estimate an opacity of τ> 2 toward the central position. It could be even larger for a higher carbon isotopic ratio (Martín et al. 2010). This shows that in the central position, the HCN emission either stems from regions significantly smaller than the beam, or the carbon isotopic ratio is significantly smaller in this region. We cannot disentangle these two possibilities with our data. Though this uncertainty on the source size may have a moderate impact in the relative abundances of the brightest species, we have no further clues on the actual molecular clump source sizes across the galaxy so we assume a similar source size for all positions as a first approximation.

The derived column densities and upper limits are listed in Table 3 for all selected positions and detected species. We note that both H13CO+ and SO detections are at the edge of detection. SO does not even show up in the integrated maps (Sect. 3), while the moment 0 detection of H13CO+ might be the result of SiO contamination. Derived column densities for these two species are ~3σ in the few positions where those are detected, and it results in an overabundance of H13CO+ in position E of a factor of ~4 which may indicate the fit to be dominated by an spurious spectral artifact (see fit in Fig. 3). Thus these species will not be included in the following discussion.

3.3. Relative molecular abundances

We aim to understand the chemical differentiation between the molecular gas in the SF ring and the material in the close vicinity of the nuclear engine. The central few hundred parsecs circumnuclear disk (CND) contains a significant fraction of the dense molecular gas in NGC 1097 (Table 3). Based on the integrated intensity maps of HCN and HCO+ in Fig. 2 the central 600 pc region encloses 32% and 25% of the total detected emission, respectively. This fraction is as much as 40% for CS or CCH. However, we are mostly interested in the relative abundances between the different molecular species so to determine whether an AGN driven chemistry can be claimed in the central region.

We used the brightest species in our observations, namely HCN, as a reference column density baseline. Figure 4 shows the abundances of each species relative to HCN. Molecules are displayed in decreasing order of abundance as measured in position A. To better evaluate the differences between position A and those in the SF ring, we have normalized the relative abundances to those in position A (lower panel in Fig. 4).

The selection of a good “baseline” species for normalization is important but not critical in our study. As noted by Kohno et al. (2003), HCN is observed to be significantly enhanced toward the nucleus relative to CO which might point out HCN as a not the ideal candidate to become a reference molecule. However, this HCN/CO trend gets less evident when higher J transitions of CO are considered (Hsieh et al. 2012).

We see in Fig. 4 that CS is consistently slightly more abundant in the star forming ring positions. This could be caused by the normalization by HCN, implying an slight overabundance of HCN in the nuclear region as previously claimed as an AGN chemical imprint. Therefore, another possibility among the brightest species would have been the use of CS, as done in previous works (Martín et al. 2009a, 2011; Aladro et al. 2011a, 2013). However, we note that reproducing Fig. 4 with the abundances relative to CS results in an overall underabundances of all species detected in the SF ring compared to position A. Given that, a priori, we have no reasons to assume all species to be overabundant in the CND, we stick to our use of HCN as it does provide abundances less biased toward the AGN position. However, this uncertainty in the reference species is taken into account in the following discussion.

Though we will deal with relative abundance among species, for completeness we used the molecular hydrogen column densities derived from CO observations by Hsieh et al. (2011) to estimate the fractional abundances relative to H2. On average the estimated fractional abundances of HCN would be X(HCN) ≳ 1−2 × 10-9 both in the nuclear region and throughout the SF ring. We consider this a limit given that they use the conversion factor XCO = 3 × 1020 cm-2 (K km s-1)-1 which is known to be overestimating of the H2 column density in dense environments. Thus the relative abundance could be as high as X(HCN) ~ 10-8.

4. SF ring versus AGN abundances

We find that the overall relative molecular abundances in the SF ring positions are in significantly good agreement with those in the nuclear region within less than a factor of 2. The only exception is the underabundance of HNCO in some SF ring positions. Though we do not find enormous differences in the abundances among the selected positions, some species appear to show a differentiation between their abundances in the surroundings of the AGN and the positions in the star forming dominated ring. In particular, HC3N and HNCO appear to be the species showing the largest enhancement in the nuclear region. In the following we further discuss the differences observed.

4.1. HCO+ and CS

The relative abundances of HCO+ and CS derived in the individual SF ring positions are found to be consistently, but still marginally regarding the excitation uncertainties, ~20–50% above those found toward the AGN position.

These two molecules are claimed to be enhanced by UV radiation in the surroundings of star forming regions. Though its abundance may be equally enhanced by X-ray irradiation, HCO+ is shown to be abundant in the presence of UV fields (Bayet et al. 2008, 2011) and therefore it could be associated to the massive star formation. Additionally, HCO+ is also observed to be enhanced in high velocity shocked material as observed in Galactic supernovae remnants (Dickinson et al. 1980; Wootten 1981) which, again would link its enhancement to massive star formation. High abundances of CS may be understood through the enhancement of its precursor S+ in the gas phase(Drdla et al. 1989; Goicoechea et al. 2006), though there is some disagreement between theoretical models and observations (Martín et al. 2008; Tideswell et al. 2010).

Both HCO+ and CS follow closely the emission of HCN, and therefore they may be just probing the same dense gas. We do not observe a clear morphological differentiation with respect to HCN at our achieved resolution in the SF ring so as to attribute their emission to the star formation in the region. However, the significant star formation in the ring could explain their overall significantly enhanced emission with respect to the central region. We observe an HCN/HCO+ ratio which is higher, both in the AGN and the SF ring, than what is measured in other starburst galaxies (Krips et al. 2008). Rather than a general enhancement of HCN in this NGC 1097 due to the presence of the AGN, it is likely that in starbursting galaxies HCO+ is further enhanced due to the star formation event. In such SF dominated environments, ionization due to cosmic rays accelerated in supernovae remnants (Ackermann et al. 2013) would also contribute to pull HCN/HCO+ down (Wootten 1981) compared to what is observe even in the moderately SF ring on NGC 1097, or similarly in NGC 1068. This scenario may as well explain why this ratio is moderately lower in the SF ring than in the very nuclear region, while the highest HCN/HCO+ ratio would be a local effect in the central region as discussed in the following.

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Integrated intensity HCN-to-HCO+ line ratio. Values only above 5σ in the individual integrated images has been used in this map. The position of the peak of molecular emission is shown with a cross. Synthesized beam size is represented in the bottom left corner.

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4.1.1. AGN Irradiation? HCN/HCO+ ratio

For more than a decade now, it has been claimed that the X-ray irradiation in AGN dominated galaxies results in an enhancement of the HCN molecule relative to the overall molecular gas traced by CO or that affected by star formation traced by HCO+ (Kohno et al. 2001; Krips et al. 2008). In terms of relative abundances, we find that the X(HCN / HCO+) = 2.7± 0.1 in the central position is only marginally larger than the values in the SF ring which range 2.1−2.7.

The high sensitivity of the ALMA data allows us to study the distribution of this ratio across the imaged region. In Fig. 5 we show HCN/HCO+ integrated line intensity ratio, following discussions in the literature. To make the most out of the high quality of the data and to avoid noise effects, we have only included points above a 5σ level in the individual images.

Regarding its comparison with the outer SF ring, a clear HCN/HCO+ integrated intensity ratio enhancement is observed in the central 300 pc region of NGC 1097, as expected in an AGN dominated environment. However, this enhancement does not reach the maximum at the central position, as discussed in Sect. 5.1. It is interesting to note that the HCN/HCO+ measured is consistently high (>1) all over the galaxy. That is, setting these values in the proposed diagnostic diagrams based on the HCN/HCO+ ratio (Krips et al. 2008), all the molecular gas in NGC 1097 would appear in the AGN dominated regime. The difference between the HCN/HCO+ in the nucleus as compared to the SF ring is less pronounced than in NGC 1068 where the ratio drops to ~1 in the ring (Viti et al. 2014). However, they only detected these species in a handful of compact positions on the SF ring, and a significant fraction of the gas in the image might be resolved out.

Extensive literature can be found where HCN is claimed to be enhanced by the effect of X-ray irradiation (see Graciá-Carpio et al. 2006; Krips et al. 2008, and references therein). A clear correlation is found between the CO-normalized X-ray flux in the 6–8 keV band and HCN emission (García-Burillo et al. 2014), which is, however, also found for HCO+, SiO and CN (García-Burillo et al. 2010). Possibilities for the HCN enhancement such as oxygen depletion are discarded based on ancillary molecular line ratios not matching the predictions (Usero et al. 2004). The enhancement due to the presence of massive star forming regions explored by Graciá-Carpio et al. (2006) for LIRGs was discarded toward NGC 1097 in view of the low star forming rate in its nuclear region (Izumi et al. 2013). However, even the X-ray enhancement appears to be out of the question (Izumi et al. 2013) given that most models assume AGN luminosities of LX ~ 1043−44 erg s-1 (Meijerink & Spaans 2005; Meijerink et al. 2007, 2013), which is more than two orders of magnitude higher than the values measured in NGC 1097 or NGC 1068. Nevertheless, intrinsic X-ray fluxes may be significantly higher. Such is the case of NGC 1068 where its nucleus is absorbed by H2 column density >1024 cm-2 (Matt et al. 1997) and its intrinsic luminosity is estimated to be a ~2 orders of magnitude larger than observed (Iwasawa et al. 1997; Colbert et al. 2002). However, in the case of NGC 1097, the absence of Fe K emission lines in its X-ray spectra completely rules out the possibility of the presence of a heavily absorbed AGN revealing an intrinsically low-luminosity AGN. In such case it is not expected that the sphere of AGN influence goes beyond a few tens of parsecs in these sources. Figure 5 shows the central region of HCN/HCO+ enhancement to be extended well beyond one synthesized beam (see Sect. 5.1). Based on the modeling by Harada et al. (2010), Izumi et al. (2013) therefore proposed high-temperature chemistry as the key to enhance HCN and therefore obtain an increase in the HCN/HCO+ ratio in the nucleus of NGC 1097. LVG analysis by Hsieh et al. (2008) based on interferometric CO 2−1 and 1−0 shows the presence of such high temperature gas (Tkin> 400 K) in the nuclear region. Similarly, the LVG analysis of a sample of AGN sources with enhanced HCN emission resulted in kinetic temperatures TK> 40 K (Krips et al. 2008) at single dish resolution. High resolution multitransition observations toward NGC 1068 show clumps in the CND with temperatures above 100 K (Krips et al. 2011; Viti et al. 2014). Regarding the origin of such heating, mechanical heating is suggested to explain the required high temperature in NGC 1097 (Loenen et al. 2008; Izumi et al. 2013).

A more detailed exploration of the variation of this ratio as the gas approaches the central engine is found in Sect. 5.

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HCN/HCO+ and HCN/CS ratios calculated for the observable transitions in the ALMA band 3 (HCN and HCO+1−0, and CS 2−1) and band 7 (HCN and HCO+J = 4−3, and CS J = 7−6) as a function of the LTE excitation temperature. The curves have been calculated to reproduce the observed integrated line ratios for Tex = 8 K.

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4.1.2. The HCN/CS diagnostic

Recently, Izumi et al. (2013) proposed an AGN vs. SB diagnostic diagram based on the HCN(J = 4−3)/CS(J = 7−6) ratio. Toward NGC 1097, where the CS line was not detected down to a level of 2.6 mJy, this ratio was reported to be a factor of >3 larger than in starburst galaxies. This difference in the line ratio in AGN versus SB galaxies has also been reported at the lower-J transitions with single dish observations toward NGC 1068 compared to those in NGC 253 and M 82 (Nakajima et al. 2011; Aladro et al. 2013). Based on our 5 mJy beam-1 detection of CS J = 2−1 and assuming the LTE at Tex = 8 K, the CS J = 7−6 line would have a peak flux density of ~0.6 mJy beam-1. The fact of measuring a significantly different HCN/CS ratio between the high-J (>13) and the low-J transitions (~3) is the result of the difference between the upper energy levels of the transitions involved in the ratios. While the HCN and CS ALMA band 3 transitions have similar upper energy levels (Table. 1), there is a significant difference between that of HCN J = 4−3 (42 K) and CS J = 7−6 (65 K). Such difference makes the HCN(J = 4−3)/CS(J = 7−6) ratio very sensitive to variations in the excitation temperature defining the energy levels populations. This is illustrated in Fig. 6 where we calculated the HCN/HCO+ and HCN/CS line ratios for the transitions observable in the ALMA band 3 and 7 bands. While HCN/HCO+ ratios are basically insensitive to excitation conditions (as long as both species share the same excitation), similar to the low-J HCN/CS ratio, the high-J HCN/CS ratio shows a strong variation as a function of the excitation temperature. Thus the ratio among the high-J HCN/CS is a less reliable probe to the abundance variations if the excitation conditions are not well constraint.

Rather than rejecting the diagnostic proposed by Izumi et al. (2013) based on this ratio, our result aims at understanding the origin of the large ratio difference observed between AGN and SB galaxies. Though a small abundance difference of up to a factor of two may be claimed as is suggested by the observed difference in the low-J transition ratio (Aladro et al. 2013), the larger difference observed in the high-J ratio is likely due to the excitation of CS. In starburst galaxies, the high-J transitions of CS appear to be associated to a moderately higher excitation temperature gas component (~15–30 K, Aladro et al. 2011b). This component appears to correspond to a dense molecular component (~106 cm-3). From the results in NGC 1097, we can suggest that this dense molecular component may be less prominent in AGNs, or CS might be not so efficiently produced there. However a more complete high resolution study of the excitation of the gas in NGC 1097 and NGC 1068 should help understanding the origin of this underabundance and/or underexcitation.

4.2. Star formation: CCH

CCH is observed to vary significantly throughout the SF ring, with measured relative abundances 20% below (position B), up to a 70% above (position G) those in the center. The distribution of the emission and abundances of CCH differs significantly from other species in NGC 1097.

Within the Galaxy this species is observed to be located in the UV irradiated cloud edges associated with massive star forming regions (Beuther et al. 2008; Walsh et al. 2010; Li et al. 2012). Its formation paths are favored in photodissociation regions (PDRs) by the reaction of C+ with small hydrocarbons and additionally through photodissociation of C2H2 (Meier & Turner 2005, and references therein). However UV radiation is also its main destruction path, and therefore CCH abundance is dependent on the evolutionary stage of the star forming event (Li et al. 2012). In external galaxies the abundance of CCH appears not to be affected by the type of activity (Nakajima et al. 2011; Aladro et al. 2013). However, observations toward an extended sample of galaxies shown that CCH in AGNs may be similarly overabundant to starburst in the late stages of evolution while being different to earlier stage starbursts (Aladro et al. 2014). Overall, when the average galactic emission is observed in a sample of galaxies, a good correlation between CCH and HCO+ is found (Martín et al. 2014). However, we do not find such correlation at GMC complex scale in our data. At high resolution, observations toward starburst galaxies (Meier & Turner 2005, 2012; Meier et al. 2014) have shown CCH to be tracing UV irradiated clouds in the vicinity of both nuclear stars clusters and embedded star forming regions, showing large abundance variations across these galaxies. Similarly, we observe large relative abundances variations both in the nucleus and the SF ring in NGC 1097. Such variations might explain the observed homogeneity between different activity types where, when averaged over the whole few hundred parsecs of a galaxy, the local variations are smoothed out.

thumbnail Fig. 7

Comparison between the FUV emission (in color, Gil de Paz et al. 2007), and the HCN (gray contours) and CCH (white contours).

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Figure 7 shows a comparison between the far-ultraviolet (FUV) emission from unobscured massive star formation in the SF ring of NGC 1097 (Gil de Paz et al. 2007) with our observed HCN and CCH emission. The north-eastern region, where the brighter FUV emission is observed, does not correspond to the higher relative abundance of CCH. There (positions B and C), we find a large fraction of dense well UV-shielded gas, therefore decreasing the CCH relative abundance with respect to HCN, even though its absolute column density is as high as at other positions of the ring. Additionally the bright FUV from stars already formed would photodissociate CCH. On the other hand, the position I, also highly illuminated in the north-east, has significantly less dense molecular gas, but one of the highest CCH relative abundances showing that both evolved (strong observed UV) and ongoing stage star forming (enhanced CCH) regions co-exist in this region. That is similar to what is observed in position G toward the south. There, though the observed FUV is not so intense, likely due to extinction, it is enough to photo-enhance the abundance of CCH in a more diffuse medium, resulting in the highest CCH relative abundance measured. This scenario is similar to that proposed to explain the high CCH abundance in the isolated galaxy CIG 638 (Martín et al. 2014). Finally, toward the south-west (positions E, and F), we find a region where marginal FUV is observed, again possibly due to obscuration in this gas-rich environment. If CCH is indeed mostly enhanced in PDRs associated with massive star forming hot cores, this would be indicative of obscured star formation in this region, which is consistent with the 860 μm emission observed in these positions, also claimed to be tracing dust massive star forming regions (Izumi et al. 2013).

Though CCH can be a potential tracer of obscured star formation, its abundance variations can also be probing changes in the diffuseness of the ISM and therefore its permeability to the UV irradiation from massive stars. It is important to note that the critical density of CCH is about an order of magnitude below than that of species such as HCN so excitation effects might again play an important role in the relative abundance derived, particularly toward the densest cores.

4.3. The densest gas: SiO, HNCO and HC3N

These three species are the ones showing the clearest contrast between the central region and the SF ring with a significant enhancement toward the nuclear region. Toward NGC 1068, an enhancement of SiO and HC3N in the surroundings of the AGN was already been recently reported (García-Burillo et al. 2010; Takano et al. 2014).

SiO is only detected in one position outside the nuclear region, position E, and there it shows a relative abundance 25% lower in this position. Similarly, HNCO shows an underabundance of 30−40% in the SF ring with respect to the central position, but for position C, where HNCO shows an enhancement of 20%. Moreover the limits toward the undetected positions indicate abundances 40−80% below than that in the AGN vicinity. Both species are considered as tracers of shocked dense material where shocks release both SiO and HNCO from the dust grain surfaces (Martin-Pintado et al. 1997; Huettemeister et al. 1998; Zinchenko et al. 2000; Martín et al. 2008). The emission of both species is observed to be well correlated not only in Galactic sources, but also in nearby bright galaxies (Usero et al. 2006; Meier & Turner 2005). Surprisingly, in position E, where SiO has been detected in the SF ring, the lowest limit to the abundance of HNCO is found. This is likely linked to the different evolutionary stage of the embedded star forming cores where UV radiation or high-velocity shocks are destroying HNCO (Martín et al. 2008).

With a critical density of ~105 cm-3 (Wernli et al. 2007), HC3N is tracing the densest regions within the GMC complexes in NGC 1097. Where detected, the measured relative abundances in the SF ring are 25−50% of that in the central position. The upper limits in the other positions are still around 40−50% below. In the case of HC3N an increase in the temperature of the gas toward the central region would enhance this difference. Our calculated ratio of HC3N/HCN = 1.2 for Tex = 8 K (see Sect. 3.2) would increase by a factor of 5−6 for excitation temperatures of ~20 K.

5. Molecular variations within the central 300 pc

Figure 5 clearly suggests observable variations in the HCN/HCO+ line ratios within the CND even though the central region is only resolved over a few synthesized beams. Molecular variations in the central few hundred parsec CND around the AGN in NGC 1068 have been reported both at very high spatial resolution (35 pc, García-Burillo et al. 2014; Viti et al. 2014) for HCN and HCO+ and at a coarser spatial resolution of 300′′ × 170′′ for a wider sample of species (Takano et al. 2014). Here we discuss the different morphologies of the observed species toward NGC 1097 and compare it to what is observed in NGC 1068.

5.1. The HCN/HCO+ gradient

Within the central 300 pc we observe that the HCN/HCO+ emission does not peak toward the AGN position. On the contrary, a positive gradient is observed as we get farther from the central position (Fig. 8), reaching a relatively constant maximum value of ~2. The ratio of 1.65 at the central position is still significantly higher than the average ~1.3 measured in the SF ring (Sect. 4.1.1). The relatively low HCN/HCO+ ratio in the close vicinity of an AGN compared to its surrounding CND has also been reported toward NGC 1068 (García-Burillo et al. 2014). Their 35 pc spatial resolution result in an even more dramatic gradient from a similar value toward the center of ~1.5 up to a ratio of ~3 in some CND regions. As discussed above when comparing with the starburst ring, this gradient could be revealing the direct effect of the AGN imprinted in the molecular abundances on its immediate surroundings. However, it has been claimed that the variation of this ratio could be the result of a density gradient, or due to differences in the opacity of these species (Meier & Turner 2012; Meier et al. 2014).

Though HCN and HCO+ may be moderately optically thick (see Sect. 3.2), differential opacities are likely not to play a major role in the ratios observed where, for a similar column density, HCO+ has an opacity almost twice that of HCN due to the higher radiative efficiency of HCO+ as noted by Meier & Turner (2012). Given that both species show a similar excitation temperature (Izumi et al. 2013), a differential opacity effect might result in an increased HCN/HCO+ ratio, where HCO+ would reach saturation faster than HCN, if both species were similarly enhanced toward the central position, contrary to what is observed. On the other hand, the difference between their critical densities might suggest that HCO+ is mostly concentrated toward the nuclear region where the densities are moderate ~104.5 cm-3, with a higher density region ranging 100−200 pc around the AGN. This scenario is equivalent to that discussed toward local starbursts (Meier & Turner 2012; Meier et al. 2014), though the actual density structure and morphology is likely to differ in both galaxy types.

The last scenario is a real relative abundance radial gradient from the AGN. However it could be either due to an enhancement of HCN production outwards from the nucleus or an inwards overproduction of HCO+. The overproduction of HCO+ due to enhanced star formation is discussed in Sect. 4.1.1 and 4.2. Massive star formation could be taking place in the central 100 pc, or cosmic ray acceleration in the AGN would enhance HCO+ but we have no evidence for any of these effects. Thus, we rather claim that this gradient may be understood as a result of the enhancement of HCN in the material surrounding the circumnuclear disk (see Sect. 5.2). Based on theoretical (Pineau des Forets et al. 1990) and Galactic observations (Tafalla et al. 2010), the enhancement of HCN in the outflow of Mrk 231 has been claimed to be the result of shock chemistry (Aalto et al. 2012) where HCN is efficiently formed via the reaction CN + H2. We note that the HCN/HCO+ enhancement is observed outside the CND defined by HNCO (Sect. 5.2) and that the largest enhancement is observed in the extended HCN emission component emission. Though HCO+ shows extended emission south of the central region, HCN appears to show an even wider component extending in the north-east and south-west directions (Fig. 2). However, we do not have other strong evidence of outflowing material in our images. On the contrary, the kinematic study of HCN by Fathi et al. (2013) shows evidence of inflowing gas.

thumbnail Fig. 8

Integrated intensity HCN/HCO+ ratio as a function of the galactocentric distance. Ratio has been averaged in bins of 0.5′′ (35 pc). Error bars represent the dispersion of the values on each bin.

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5.2. The CND traced by HNCO

Even though HNCO may be one of the most fragile species in our sample, it shows an enhancement toward the central region (Sect. 4.3). This species is the only one clearly delineating a rotating circumnuclear disk around the AGN position as shown in Fig. 2. From the extreme emission peaks in the channel maps and taking into account the beam smearing, we measure a disk structure of 180 ± 40 pc length and PA = 120 ± 10°, covering a velocity range of 200 km s-1 around the systemic velocity. The measured velocity gradient of 1.1 ± 0.2 km s-1 pc-1 is consistent with that measured toward the nuclear region by Hsieh et al. (2008). The orientation of the disk is marginally smaller than the kinematic P.A. of 133°, and 146° derived from CO 2−1 (Hsieh et al. 2011) and HCN 4−3, respectively (Fathi et al. 2013). This might indicate a real variation between the overall rotation of the gas envelope traced by HCN and the inner disk traced by HNCO. The possibility of HNCO tracing a bipolar outflow rather than a disk structure is unsupported by its kinematics being closely following those of CO and HCN at larger scales. As observed in other species, the south-east region of the disk is about a factor of two brighter than the north-west one. However the slightly narrower line width at this position (~80 km s-1) makes this difference not to be apparent in the integrated maps. This is an indication of a significant asymmetrical distribution of the molecular gas in the CND (also seen in CO 2−1, Hsieh et al. 2008), similar to what is observed at higher resolution in NGC 1068 (García-Burillo et al. 2014). Also in NGC 1068, though at slightly lower resolution, the emission of HNCO is observed distributed in two lobes at both sides of the AGN (Takano et al. 2014). Such double peak distribution is in agreement with the CND being observed from a more inclined direction consistent with its Seyfert 2 nucleus.

HNCO forms in the very inner regions of molecular cloud, shielded from external UV irradiation by large visual extinction as shown by chemical models (Av> 4 mag, Martín et al. 2009b). This species is exclusively distributed along the circumnuclear rotating structure. Within the central 300 pc, HNCO is absent in the regions outside the rotation plane of the CND, unlike the brightest species HCN, HCO+, CCH and CS, which clearly show a wider extent. In this region, low velocity shocks in the ISM due to cloud to cloud collision similar to what is observed in our Galactic center (Jones et al. 2012), as well as in external galaxies (Meier & Turner 2005) will provide the environmental conditions for its ejection into gas phase while being dense enough to protect it from dissociation. Though sensitivity could be claimed for such non detection, the HCN/HNCO ratio map in Fig. 9 shows already HNCO being exclusively concentrated in the disk, with the lower ratio toward the two CND lobes, and a clear bipolar decrease in the perpendicular direction to the plane. This fact points out to an increase of the radiation affecting the gas outside the CND. Given that star formation is not prominent in this region, UV generated in high-velocity shocks might play a significant role in the destruction of HNCO, which may also explain the enhancement of HCN with increasing distance from the nucleus (Sect. 5.1). Additionally, an ionization cone due to a putative jet or direct exposure to the X-ray emission from the AGN, could be claimed together to explain the absence of HNCO within the inner region (<100 pc) enclosed by the CND and the biconical shape of the HCN/HNCO ratio map.

thumbnail Fig. 9

Integrated intensity line ratios of HCN over HCO+, HNCO, CS and CCH in the central ~500 pc of NGC 1097. Position of peak of molecular emission is marked with a cross. The 3σ contour of HNCO emission, delineating the circumnuclear disk around the AGN, is overlaid as a reference. Synthesized beam size is represented in the bottom left box.

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5.3. HC3N and SiO in the close vicinity to the AGN

Both HC3N and SiO are observed to be concentrated within an unresolved region (i.e., 150 pc) around the AGN. Such a high concentration of these molecules in the surroundings of an AGN has also been reported in NGC 1068 (García-Burillo et al. 2010; Takano et al. 2014).

Though HC3N shows some emission in the south-eastern position of the CND, the brightest in the CND, it is mostly concentrated in the central beam. Takano et al. (2014) reported that a ~70% of the HC3N emission stems from the CND in NGC 1068. Similar to what is observed in NGC 1097, HC3N is more concentrated around the AGN than molecules tracing the CND such as HNCO. Our observations together with those in NGC 1068 provide the evidence of the existence of a large amount of high density gas (~106 cm-3) shielded from the X-ray radiation from the AGN, as described by theoretical models from Harada et al. (2013). In those models, a high temperature region of the disk moderately affected by X-rays can explain an enhancement of the cyanopolyynes. In this scenario, HC3N might be tracing the inner CND directly enclosed by HNCO. Within scales almost two orders of magnitude smaller, the few central parsecs around the Galactic black hole show HC3N (and to a large extent SiO) to be tracing the very densest clumps in the circumnuclear disk material (Martín et al. 2012).

HC3N has been observed to be overluminous in the deeply buried IR luminous galaxy NGC 4418 (Aalto et al. 2007) which might be a signature of either buried star formation (Bayet et al. 2008) or contribution from gas in the vicinity of the AGN. HC3N enhancement has been confirmed in other obscured LIRGs (Costagliola et al. 2011). The observed HC3N/HCO+ integrated intensity ratio toward NGC 4418 is ~0.4–0.6 (Aalto et al. 2007; Costagliola et al. 2011). This is using the J = 10−9 transition of HC3N, and therefore the ratio would be higher if using the J = 11−10 in our work. The ratio we derive toward the nucleus of NGC 1097 is however ~0.17, and therefore significantly lower than the value in NGC 4418. Similarly, for those LIRGs where HC3N was detected in the sample from Costagliola et al. (2011), a ratio ranging HC3N/HCN ~ 0.4−0.2 is found (again using the fainter J = 10−9 HC3N transition). Toward NGC 1097 we observe a lower ratio of ~0.1. Though we know that both species are not coexistent in NGC 1097, and thus a higher ratio of HC3N might be measured toward the central position, a similar non-coexistence applies in the obscured LIRGs observed with single-dish resolution. Therefore, based on our observations, an enhancement of HC3N in the CND around a putative AGN cannot be the only contribution to the observed HC3N enhancement in obscured LIRGs. This gives a further support to the idea of buried young star formation in this objects as a key ingredient driving their luminosities (Aalto et al. 2007; Costagliola et al. 2011). We note, however, that the line ratios HC3N/HCO+ ~ 0.16 and HC3N/HCN ~ 0.1 measured toward the close IR bright quasar, Mrk 231, are in quite good agreement to those measured in the center of NGC 1097, even though the strong star formation in Mrk 231 (Aalto et al. 2012, and references therein).

On the other hand, in the CND region SiO is exclusively detected toward the central beam. Though the signal to noise of our data is not high, the SiO/H13CO+> 1 line ratio is consistent with the observations toward NGC 1068 (Usero et al. 2004). SiO is a tracer of shocks both in the Galaxy (Martin-Pintado et al. 1992, 1997; Huettemeister et al. 1998) and in external galaxies (García-Burillo et al. 2000; Usero et al. 2006). Toward NGC 1068, X-ray and cosmic ray chemistry has been claimed to explain the SiO abundance in its CND (García-Burillo et al. 2010; Aladro et al. 2013) based on the correlation between SiO emission and the Fe 6.4 keV line in the Galactic center (Martín-Pintado et al. 2000; Amo-Baladrón et al. 2009). However, the high abundance of the easily destroyed HC3N would not resist photodissociation in such environment. Still, the emission could be enhanced by the X-ray radiation in a region different to that where HC3N is formed (Harada et al. 2013), which might explain the enhanced abundance of both species. The signal-to-noise ratio of our SiO detection prevents us from reaching further conclusions, but to confirm the compact SiO emission in the surroundings of AGN, similar to what is observed in NGC 1068 (García-Burillo et al. 2010).

5.4. CS and CCH

As shown in Fig. 9, the behavior of these two species in the central few hundred parsecs appear to anticorrelate. Though the resolution is limited, based on previous studies and theoretical models we suggest that such differentiation is likely to be due to real abundance differences caused by environmental conditions.

CS is observed to be evenly distributed across the CND, with a relative abundance drop of almost a factor of two in the south-eastern CND region (observed peak of HCN/CS ratio in Fig. 9), contrary to what is observed in CCH. Though its abundance varies, CS seems to be abundant in the CND and not prominent in the region outside that plane.

Our observations show the CCH to be more abundant (lower HCN/CCH ratio in Fig. 9) toward the south-east CND region where the peak line emission is found for most species, with a significant but not too prominent (~60%) relative abundance decrease toward the north-western part of the CND. In addition its abundance is also significant outside of the CND plane defined by HNCO, which might be linked to outflowing material similar to what is observed in Maffei 2 (Meier & Turner 2012). The differences observed might be due to temperature affecting its chemistry. The models from Harada et al. (2013) (for the smaller XDR fraction to better represent this low-luminosity AGN) show CCH abundance to decrease as the temperature increase.

6. Summary

In this paper we have presented the 3 mm molecular observations carried out with ALMA toward NGC 1097. The detection of eight different molecular species has been discussed under our current understanding of the formation and excitation of each of these species. We have developed a molecular scenario of NGC 1097 first between the star forming ring and the nuclear region and secondly regarding the barely resolved morphology of the emission of these molecules in the central ~300 pc.

The highest concentration of dense gas is located in the surroundings of the AGN (Hsieh et al. 2012; Izumi et al. 2013). The species HCN, HCO+ and CS appear to be tracing the same molecular component. An increase of the abundance of HCO+ and CS relative to HCN of 20−50% in the star forming ring with respect to the central region is observed. The claimed large discrepancy in the HCN/CS ratio between SB and AGN galaxies (Izumi et al. 2013) is likely due to a real underabundance of CS of a factor of ~2 together with excitation differences. CS is observed to be excited to higher temperatures (Aladro et al. 2011b), which may be the evidence of a more prominent high density component (106 cm-3) in SBs and may be less significant in AGNs. Additionally, CS could be underproduced in this high density regions in AGNs.

CCH shows overabundances of up to 70% in the SF ring, and its abundance distribution differs significantly from the other species. We claim it to be closely related to star formation and it might be a good tracer of obscured star formation in the ring. The largest abundance contrast is shown by the densest gas tracers, namely SiO, HNCO, and HC3N, which are clearly overabundant around the AGN.

Within the central ~300 pc HNCO clearly delineates a circumnuclear disk of 180 ± 40 pc around the nucleus. The disk PA = 120 ± 10° is slightly less inclined than the rotation plane of the overall molecular gas in the central region (PA = 133−146°, Hsieh et al. 2011; Fathi et al. 2013). This disk appear to enclose the emission of HC3N and SiO which suggest an stratification of the disk as predicted by models (Harada et al. 2013) with each species being formed/enhanced at different regions within the disk. In this scenario, HNCO would trace the core of the molecular clouds in the disk well protected from the radiation from the AGN. Inside we would find a dense region moderately exposed to X-ray radiation where HC3N would be enhanced. Finally the radiation resilient SiO might be tracing the innermost molecular region of the circumnuclear disk.

HCN/HCO+ shows a positive gradient as we move away from the AGN, similar to what is observed toward NGC 1068, and therefore an enhancement of HCN via X-ray from the AGN is discarded. Unless HCO+ has some mechanism to be enhanced in the close vicinity of the AGN, we find plausible the HCN enhancement off the circumnuclear disk plane due to shocked gas in outflowing material from the central engine.

The results presented in this paper toward the low luminosity AGN in NGC 1097 are in agreement with previous results on the luminous AGN on NGC 1068 (García-Burillo et al. 2014; Takano et al. 2014), thus the difference in luminosity between the two sources does not appear to have a impact on its chemical structure around their AGNs. These early science ALMA results clearly show the potential of chemical studies to understand the physical processes in the circumnuclear disks around AGNs.


Acknowledgments

This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00108.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ.

References

All Tables

Table 1

Spectral parameters of detected transitions.

Table 2

Coordinates and line parameters of extracted spectra.

Table 3

Column densities for each species and the selected position.

All Figures

thumbnail Fig. 1

Full spectral coverage of the ALMA Band 3 observations extracted from the nuclear position of NGC 1097 where the peak of molecular emission is observed for all species. This position corresponds to position A in Table 2 and Fig. 2.

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In the text
thumbnail Fig. 2

Moment 0 maps of all detected species in the velocity range [900−1600] km s-1, except for CCH where a range [600−1600] km s-1 was used to include the two groups of hyperfine components. The 1σ noise level in the integrated maps is 62 mJy km s-1 for all species, but for CCH which is 77 mJy km s-1. Logarithmic color scale is set to allow a direct comparison of the emission of the different species. Color levels are set to a minimum of 0.1 mJy km s-1 so that emission over 3σ level is seen above the black background. Positions where spectra were extracted are marked in all boxes, and labeled in the upper left box.

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In the text
thumbnail Fig. 3

Spectra extracted from selected positions in the AGN position (A) and on the SF ring (B-I) of NGC 1097. Frequency span has been cropped with respect to that of Fig. 1 removing the line free frequencies at the edges of both sidebands. Flux density scale has been multiplied by a factor of ×4 in the regions (defined by the vertical dashed lines) containing the fainter lines to improve their visualization. Molecular fit to the observed emission is represented by the red line. Non-detections are presented as the 3σ limit Gaussian profiles.

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In the text
thumbnail Fig. 4

Top: molecular abundances relative to HCN estimated in the sample of selected positions for all detected species. Colored histograms represent species detected while empty histograms represent upper limits to the detection. Bottom: abundances normalized to those of position A for comparison. As a reference, the three horizontal dotted lines represent equal relative abundances or a factor of two above and below those in position A.

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In the text
thumbnail Fig. 5

Integrated intensity HCN-to-HCO+ line ratio. Values only above 5σ in the individual integrated images has been used in this map. The position of the peak of molecular emission is shown with a cross. Synthesized beam size is represented in the bottom left corner.

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In the text
thumbnail Fig. 6

HCN/HCO+ and HCN/CS ratios calculated for the observable transitions in the ALMA band 3 (HCN and HCO+1−0, and CS 2−1) and band 7 (HCN and HCO+J = 4−3, and CS J = 7−6) as a function of the LTE excitation temperature. The curves have been calculated to reproduce the observed integrated line ratios for Tex = 8 K.

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In the text
thumbnail Fig. 7

Comparison between the FUV emission (in color, Gil de Paz et al. 2007), and the HCN (gray contours) and CCH (white contours).

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In the text
thumbnail Fig. 8

Integrated intensity HCN/HCO+ ratio as a function of the galactocentric distance. Ratio has been averaged in bins of 0.5′′ (35 pc). Error bars represent the dispersion of the values on each bin.

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In the text
thumbnail Fig. 9

Integrated intensity line ratios of HCN over HCO+, HNCO, CS and CCH in the central ~500 pc of NGC 1097. Position of peak of molecular emission is marked with a cross. The 3σ contour of HNCO emission, delineating the circumnuclear disk around the AGN, is overlaid as a reference. Synthesized beam size is represented in the bottom left box.

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In the text

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