First detections of extragalactic SO<sub>2</sub>, NS and NO

Martín, S.; Mauersberger, R.; Martı́n-Pintado, J.; García‐Burillo, S.; Henkel, C.

doi:10.1051/0004-6361:20031442

Cited by 68 publications

(59 citation statements)

References 18 publications

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“…Some other faint shock tracers have only been detected in this galaxy, such as HOCO + and NS, as well as the sulphur bearing species SO 2 . H 2 CS, and C 2 S (Martín et al 2003 which are confirmed here (see Fig. 6).…”

Section: Starburst Galaxiessupporting

confidence: 87%

Lambda = 3 mm line survey of nearby active galaxies

Aladro

Martín

Riquelme

et al. 2015

A&A

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111

188

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Aims. We aim to better understand the imprints that the nuclear activity in galaxies leaves in the molecular gas. Methods. We used the IRAM 30 m telescope to observe the frequency range ∼[86−116] GHz towards the central regions of the starburst galaxies M 83, M 82, and NGC 253, the galaxies hosting an active galactic nucleus (AGN) M 51, NGC 1068, and NGC 7469, and the ultra-luminous infrared galaxies (ULIRGs) Arp 220 and Mrk 231. Assuming local thermodynamic equilibrium (LTE), we calculated the column densities of 27 molecules and 10 isotopologues (or their upper limits in case of non-detections).Results. Among others, we report the first tentative detections of CH 3 CHO, HNCO, and NS in M 82 and, for the first time in the extragalactic medium, HC 5 N in NGC 253. Hα recombination lines were only found in M 82 and NGC 253. Vibrationally excited lines of HC 3 N were only detected in Arp 220. CH 3 CCH emission is only seen in the starburst-dominated galaxies. By comparison of the fractional abundances among the galaxies, we looked for the molecules that are best suited to characterise the chemistry of each group of galaxies (starbursts, AGNs and ULIRGs), as well as the differences among galaxies within the same group. Conclusions. Suitable species for characterising and comparing starburst galaxies are CH 3 OH and HNCO as tracers of large-scale shocks, which dominate early to intermediate starburst stages, and CH 3 CCH, c-C 3 H 2 , and HCO as tracers of UV fields, which control the intermediate-to-old or post starburst phases. M 83 shows signs of a shock-dominated environment. NGC 253 is characterised by both strong shocks and some UV fields. M 82 stands out for its bright photo-dissociated region tracers, which indicate an UV fielddominated environment. Regarding AGNs, the abundances of HCN and CN (previously claimed as enhanced in AGNs) in M 51 are similar to those in starburst galaxies, while the HCN/HCO + ratio is high in M 51 and NGC 1068, but not in NGC 7469. We did not find a correlation between the HCN/CS ratio (recently claimed as a possible starburst/AGN discriminator) and the AGN activity. However, a high enough spatial resolution to separate their circumnuclear disks from the surrounding star-forming regions is needed to find molecular abundance trends in AGNs. High abundances of H 13 CN and HC 3 N, as well as a similarity between the column densities of 13 CO and C 18 O, are representative of the molecular interstellar medium in the ULIRGs. Furthermore, the chemistry of Arp 220 points towards a more starburst-dominated environment, while that of Mrk 231 more resembles the AGNs of our sample.

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Section: Starburst Galaxiessupporting

confidence: 87%

Lambda = 3 mm line survey of nearby active galaxies

Aladro

Martín

Riquelme

et al. 2015

A&A

Self Cite

111

188

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“…Martín et al (2003) estimated a ratio NS/CS = 0.4 in NGC 253, which they interpreted as the signature of NS chemical enhancement by shocks (see also Viti et al 2001). …”

Section: B19 Nsmentioning

confidence: 97%

Molecules atz= 0.89

Müller

Beelen

Guèlin

et al. 2011

A&A

164

284

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We present the results of a 7 mm spectral survey of molecular absorption lines originating in the disk of a z = 0.89 spiral galaxy located in front of the quasar PKS 1830−211. Our survey was performed with the Australia Telescope Compact Array and covers the frequency interval 30-50 GHz, corresponding to the rest-frame frequency interval 57-94 GHz. A total of 28 different species, plus 8 isotopic variants, were detected toward the south-west absorption region, located about 2 kpc from the center of the z = 0.89 galaxy, which therefore has the largest number of detected molecular species of any extragalactic object so far. The results of our rotation diagram analysis show that the rotation temperatures are close to the cosmic microwave background temperature of 5.14 K that we expect to measure at z = 0.89, whereas the kinetic temperature is one order of magnitude higher, indicating that the gas is subthermally excited. The molecular fractional abundances are found to be in-between those in typical Galactic diffuse and translucent clouds, and clearly deviate from those observed in the dark cloud TMC 1 or in the Galactic center giant molecular cloud Sgr B2. The isotopic ratios of carbon, nitrogen, oxygen, and silicon deviate significantly from the solar values, which can be linked to the young age of the z = 0.89 galaxy and a release of nucleosynthesis products dominated by massive stars. Toward the north-east absorption region, where the extinction and column density of gas is roughly one order of magnitude lower than toward the SW absorption region, only a handful of molecules are detected. Their relative abundances are comparable to those in Galactic diffuse clouds. We also report the discovery of several new absorption components, with velocities spanning between −300 and +170 km s −1 . Finally, the line centroids of several species (e.g., CH 3 OH, NH 3 ) are found to be significantly offset from the average velocity. If caused by a variation in the proton-to-electron mass ratio μ with redshift, these offsets yield an upper limit | Δμ μ | < 4×10 −6 , which takes into account the kinematical noise produced by the velocity dispersion measured from a large number of molecular species.

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“…Studies have shown that the chemical differentiation observed within Galactic molecular clouds is also seen at larger (∼100 pc) scales in nearby galaxies (e.g., Henkel et al 1987;Nguyen-Q-Rieu et al 1991;Martín et al 2003;Usero et al 2004;Tacconi et al 2008;Pérez-Beaupuits et al 2007Baan et al 2010;van der Werf et al 2010). …”

Section: Introductionmentioning

confidence: 98%

The Structure and Dynamics of an Active Galactic Nucleus Torus: Co Line Predictions for Alma From Three-Dimensional Hydrodynamical Simulations With X-Ray-Driven Chemistry

Pérez-Beaupuits¹,

Wada²,

Spaans³

2011

ApJ

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Several attempts have been made to model the mass distribution and dynamical evolution of the circumnuclear gas in active galactic nuclei (AGNs). However, chemical evolution is not included in detail in three-dimensional (3D) hydrodynamic simulations. The X-ray radiation from the AGN can drive the gas chemistry and affect the thermodynamics, as well as the excitation of the interstellar medium. Therefore, we estimate the effects (on chemical abundances and excitation) of X-ray irradiation by the AGN for atomic and molecular gas in a 3D hydrodynamic model of an AGN torus. We obtain the abundances of various species from an X-ray chemical model. A 3D radiative transfer code estimates the level populations, which result in line intensity maps. Predictions for the CO J = 1 → 0 to J = 9 → 8 lines indicate that mid-J CO lines are excellent probes of density and dynamics in the central ( 60 pc) region of the AGN in contrast to the low-J CO lines. Analysis of the X CO /α conversion factors shows that only the higher J CO lines can be used for gas mass determination in AGN tori. The [C ii] 158 μm emission traces mostly the hot (T k > 1000 K) central region of the AGN torus. The [C ii] 158 μm line will be useful for ALMA observations of high-redshift (z 1) AGNs. The spatial scales ( 0.25 pc) probed with our simulations match the size of the structures that ALMA will resolve in nearby ( 45 Mpc at 0. 01) galaxies.

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First detections of extragalactic SO₂, NS and NO

Cited by 68 publications

References 18 publications

Lambda = 3 mm line survey of nearby active galaxies

Lambda = 3 mm line survey of nearby active galaxies

Molecules atz= 0.89

The Structure and Dynamics of an Active Galactic Nucleus Torus: Co Line Predictions for Alma From Three-Dimensional Hydrodynamical Simulations With X-Ray-Driven Chemistry

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First detections of extragalactic SO2, NS and NO

Cited by 68 publications

References 18 publications

Lambda = 3 mm line survey of nearby active galaxies

Lambda = 3 mm line survey of nearby active galaxies

Molecules atz= 0.89

The Structure and Dynamics of an Active Galactic Nucleus Torus: Co Line Predictions for Alma From Three-Dimensional Hydrodynamical Simulations With X-Ray-Driven Chemistry

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First detections of extragalactic SO₂, NS and NO