Molecules as tracers of galaxy evolution: an EMIR survey

Costagliola, F.; Aalto, S.; Rodríguez, Mónica; Müller, S.; Spoon, H. W. W.; Martín, S.; Pérez-Torres, M. A.; Alberdi, A.; Lindberg, Johan E.; Batejat, F.; Jütte, E.; Werf, P. van der; Lahuis, F.

doi:10.1051/0004-6361/201015628

Cited by 147 publications

(262 citation statements)

References 44 publications

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“…Therefore, based on our observations, an enhancement of HC 3 N in the CND around a putative AGN cannot be the only contribution to the observed HC 3 N 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 HC 3 N/HCO + ∼ 0.16 and HC 3 N/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).…”

Section: The Cnd Traced By Hncosupporting

confidence: 62%

“…HC 3 N enhancement has been confirmed in other obscured LIRGs (Costagliola et al 2011). The observed HC 3 N/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 HC 3 N, and therefore the ratio would be higher if using the J = 11−10 in our work.…”

Section: The Cnd Traced By Hncomentioning

confidence: 81%

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Multimolecule ALMA observations toward the Seyfert 1 galaxy NGC 1097

Martín

Kohno

Izumi

et al. 2015

A&A

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Context. The nearby Sy 1 galaxy NGC 1097 represents an ideal laboratory for exploring the molecular chemistry in the surroundings of an active galactic nucleus (AGN). Aims. Exploring the distribution of different molecular species allows us to understand the physical processes affecting the interstellar medium both in the AGN vicinity and in the outer star forming molecular ring. Methods. We carried out 3 mm ALMA observations that include seven different molecular species, namely HCN, HCO + , CCH, CS, HNCO, SiO, HC 3 N, and SO, as well as the 13 C isotopologues of the first two. Spectra were extracted from selected positions and all species were imaged over the central 2 kpc (∼30 ) of the galaxy at a resolution of ∼2.2 × 1.5 (150 pc × 100 pc). Results. HCO + and CS appear to be slightly enhanced in the star forming ring. CCH shows the largest variations across NGC 1097 and is suggested to be a good tracer of both obscured and early stage star formation. HNCO, SiO, and HC 3 N are significantly enhanced in the inner circumnuclear disk surrounding the AGN. Conclusions. Differences in the molecular abundances are observed between the star forming ring and the inner circumnuclear disk. We conclude that the HCN/HCO + and HCN/CS differences observed between AGN-dominated and starburst (SB) galaxies are not due to a HCN enhancement due to X-rays, but rather this enhancement is produced by shocked material at distances of 200 pc from the AGN. Additionally, we claim that lower HCN/CS is a combination of a small underabundance of CS in AGNs, together with excitation effects, where a high density gas component (∼10 6 cm −3 ) may be more prominent in SB galaxies. However, the most promising are the differences found among the dense gas tracers that, at our modest spatial resolution, seem to outline the physical structure of the molecular disk around the AGN. In this picture, HNCO probes the well-shielded gas in the disk, surrounding the dense material moderately exposed to the X-ray radiation traced by HC 3 N. Finally SiO might be the innermost molecule in the disk structure.

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Section: The Cnd Traced By Hncosupporting

confidence: 62%

Section: The Cnd Traced By Hncomentioning

confidence: 81%

Multimolecule ALMA observations toward the Seyfert 1 galaxy NGC 1097

Martín

Kohno

Izumi

et al. 2015

A&A

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“…At millimeter wavelengths, HCN has been found to be enhanced over HCO + in ULIRGs (Graciá-Carpio et al 2006) and in Seyferts over starbursts (Imanishi et al 2007), and this has been proposed to be a diagnostic of AGN activity. Costagliola et al (2011), however, argue that for high densities and columns HCO + is expected to be stronger than HCN in XDRs (Meijerink et al 2007). Models by Meijerink & Spaans (2005) predict HCN abundances and cumulative column densities in XDRs that fall by far too short to explain the values we derive in both NGC 4418 and Arp 220.…”

Section: Model Uncertaintiesmentioning

confidence: 95%

Herschel/PACS spectroscopy of NGC 4418 and Arp 220: H₂O, H₂¹⁸O, OH,¹⁸OH, O I, HCN, and NH₃

González-Alfonso

Fischer

Graciá-Carpio

et al. 2012

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Full range Herschel/PACS spectroscopy of the (ultra)luminous infrared galaxies NGC 4418 and Arp 220, observed as part of the SHINING key programme, reveals high excitation in H 2 O, OH, HCN, and NH 3 . In NGC 4418, absorption lines were detected with E lower > 800 K (H 2 O), 600 K (OH), 1075 K (HCN), and 600 K (NH 3 ), while in Arp 220 the excitation is somewhat lower. While outflow signatures in moderate excitation lines are seen in Arp 220 as have been seen in previous studies, in NGC 4418 the lines tracing its outer regions are redshifted relative to the nucleus, suggesting an inflow withṀ 12 M yr −1 . Both galaxies have compact and warm (T dust 100 K) nuclear continuum components, together with a more extended and colder component that is much more prominent and massive in Arp 220. A chemical dichotomy is found in both sources: on the one hand, the nuclear regions have high H 2 O abundances, ∼10 −5 , and high HCN/H 2 O and HCN/NH 3 column density ratios of 0.1−0.4 and 2−5, respectively, indicating a chemistry typical of evolved hot cores where grain mantle evaporation has occurred. On the other hand, the high OH abundance, with OH/H 2 O ratios of ∼0.5, indicates the effects of X-rays and/or cosmic rays. The nuclear media have high surface brightnesses ( 10 13 L /kpc 2 ) and are estimated to be very thick (N H 10 25 cm −2 ). While NGC 4418 shows weak absorption in H 18 2 O and 18 OH, with a 16 O-to-18 O ratio of 250−500, the relatively strong absorption of the rare isotopologues in Arp 220 indicates 18 O enhancement, with 16 O-to-18 O of 70−130. Further away from the nuclear regions, the H 2 O abundance decreases to 10 −7 and the OH/H 2 O ratio is reversed relative to the nuclear region to 2.5−10. Despite the different scales and morphologies of NGC 4418, Arp 220, and Mrk 231, preliminary evidence is found for an evolutionary sequence from infall, hot-core like chemistry, and solar oxygen isotope ratio to high velocity outflow, disruption of the hot core chemistry and cumulative high mass stellar processing of 18 O.

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“…No obvious correlation between these young SSCs (5−15 Myr) and the CO can be found ). In addition, both minor mergers have a relatively high CO/HCN line ratio (CO/HCN (NGC 1614) ∼ 43, CO/HCN (NGC 4194) ∼ 61; Costagliola et al 2011), which indicates limited reservoirs of dense gas.…”

Section: Comparison With Other Dust Lane Minor Mergersmentioning

confidence: 99%

The NGC 1614 interacting galaxy

König

Aalto

Müller

et al. 2013

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Minor mergers frequently occur between giant and gas-rich low-mass galaxies and can provide significant amounts of interstellar matter to refuel star formation and power active galactic nuclei (AGN) in the giant systems. Major starbursts and/or AGN result when fresh gas is transported and compressed in the central regions of the giant galaxy. This is the situation in the starburst minor merger NGC 1614, whose molecular medium we explore at half-arcsecond angular resolution through our observations of 12 CO (2−1) emission using the Submillimeter Array (SMA). We compare our 12 CO (2−1) maps with optical and Paα, Hubble Space Telescope and high angular resolution radio continuum images to study the relationships between dense molecular gas and the NGC 1614 starburst region. The most intense 12 CO emission occurs in a partial ring with ∼230 pc radius around the center of NGC 1614, with an extension to the northwest into the dust lane that contains diffuse molecular gas. We resolve ten giant molecular associations (GMAs) in the ring, which has an integrated molecular mass of ∼8 × 10 8 M . Our interferometric observations filter out a large part of the 12 CO (1−0) emission mapped at shorter spacings, indicating that most of the molecular gas is diffuse and that GMAs only exist near and within the circumnuclear ring. The molecular ring is uneven with most of the mass on the western side, which also contains GMAs extending into a pronounced tidal dust lane. The spatial and kinematic patterns in our data suggest that the northwest extension of the ring is a cosmic umbilical cord that is feeding molecular gas associated with the dust lane and tidal debris into the nuclear ring, which contains the bulk of the starburst activity. The astrophysical process for producing a ring structure for the final resting place of accreted gas in NGC 1614 is not fully understood, but the presence of numerous GMAs suggests an orbit-crowding or resonance phenomenon. There is some evidence that star formation is progressing radially outward within the ring, indicating that a self-triggering mechanism may also affect star formation processes. The net result of this merger therefore very likely increases the central concentration of stellar mass in the NGC 1614 remnant giant system.

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Molecules as tracers of galaxy evolution: an EMIR survey

Cited by 147 publications

References 44 publications

Multimolecule ALMA observations toward the Seyfert 1 galaxy NGC 1097

Multimolecule ALMA observations toward the Seyfert 1 galaxy NGC 1097

Herschel/PACS spectroscopy of NGC 4418 and Arp 220: H₂O, H₂¹⁸O, OH,¹⁸OH, O I, HCN, and NH₃

The NGC 1614 interacting galaxy

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Molecules as tracers of galaxy evolution: an EMIR survey

Cited by 147 publications

References 44 publications

Multimolecule ALMA observations toward the Seyfert 1 galaxy NGC 1097

Multimolecule ALMA observations toward the Seyfert 1 galaxy NGC 1097

Herschel/PACS spectroscopy of NGC 4418 and Arp 220: H2O, H218O, OH,18OH, O I, HCN, and NH3

The NGC 1614 interacting galaxy

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Herschel/PACS spectroscopy of NGC 4418 and Arp 220: H₂O, H₂¹⁸O, OH,¹⁸OH, O I, HCN, and NH₃