@article {214, title = {{Exploring the molecular chemistry and excitation in obscured luminous infrared galaxies: An ALMA mm-wave spectral scan of NGC 4418}}, journal = {ArXiv e-prints}, year = {2015}, keywords = {Astrophysics - Astrophysics of Galaxies}, author = {Costagliola, F. and Sakamoto, K. and Muller, S. and Mart{\'\i}n, S. and Aalto, S. and Harada, N. and van der Werf, P. and Viti, S. and Garcia-Burillo, S. and Spaans, M.} } @article {2015A\&A...574A..85A, title = {{High resolution observations of HCN and HCO$^{+}$J = 3-2 in the disk and outflow of Mrk 231. Detection of vibrationally excited HCN in the warped nucleus}}, journal = {Astronomy and Astrophysics}, volume = {574}, year = {2015}, month = {feb}, pages = {A85}, abstract = {
Aims: Our goal is to study molecular gas properties in nuclei and large scale outflows/winds from active galactic nuclei (AGNs) and starburst galaxies.
Methods: We obtained high resolution (0.{\#779}25 to 0.{\#779}90) observations of HCN and HCO$^{+}$J = 3 {\rarr} 2 of the ultraluminous QSO galaxy Mrk 231 with the IRAM Plateau de Bure Interferometer (PdBI).
Results: We find luminous HCN and HCO$^{+}$J = 3 {\rarr} 2 emission in the main disk and we detect compact (r {\l}sim} 0{\textquoteright}{\textquoteright}\&dotbelow;1 (90 pc)) vibrationally excited HCN J = 3 {\rarr} 2{$ν$}$_{2}$ = 1f emission centred on the nucleus. The velocity field of the vibrationally excited HCN is strongly inclined (position angle PA = 155{\deg}) compared to the east-west rotation of the main disk. The nuclear (r {\l}sim} 0.{\#779}1) molecular mass is estimated to 8 {\times} 10$^{8}$ M$_{\&sun;}$ with an average N(H$_{2}$) of 1.2 {\times} 10$^{24}$ cm$^{-2}$. Prominent, spatially extended ({\gsim}350 pc) line wings are found for HCN J = 3 {\rarr} 2 with velocities up to {\plusmn} 750 km s$^{-1}$. Line ratios indicate that the emission is emerging in dense gas n = 10$^{4}$-5 {\times} 10$^{5}$ cm$^{-3}$ of elevated HCN abundance X(HCN) = 10$^{-8}$-10$^{-6}$. The highest X(HCN) also allows for the emission to originate in gas of more moderate density. We tentatively detect nuclear emission from the reactive ion HOC$^{+}$ with HCO$^{+}$/HOC$^{+}$ = 10-20.
Conclusions: The HCN {$ν$}$_{2}$ = 1f line emission is consistent with the notion of a hot, dusty, warped inner disk of Mrk 231 where the {$ν$}$_{2}$ = 1f line is excited by bright mid-IR 14 {$μ$}m continuum. We estimate the vibrational temperature T$_{vib}$ to 200-400 K. Based on relative source sizes we propose that 50\% of the main HCN emission may have its excitation affected by the radiation field through IR pumping of the vibrational ground state. The HCN emission in the line wings, however, is more extended and thus likely not strongly affected by IR pumping. Our results reveal that dense clouds survive (and/or are formed) in the AGN outflow on scales of at least several hundred pc before evaporating or collapsing. The elevated HCN abundance in the outflow is consistent with warm chemistry possibly related to shocks and/or X-ray irradiated gas. An upper limit to the mass and momentum flux is 4 {\times} 10$^{8}$ M$_{\&sun;}$ and 12L$_{AGN}$/c, respectively, and we discuss possible driving mechanisms for the dense outflow. Based on observations carried out with the IRAM Plateau de Bure Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain).The reduced data cubes are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/574/A85}, keywords = {galaxies: active, galaxies: evolution, galaxies: individual: Mrk 231, ISM: jets and outflows, ISM: molecules, quasars: general}, doi = {10.1051/0004-6361/201423987}, url = {http://adsabs.harvard.edu/abs/2015A\%26A...574A..85A}, author = {Aalto, S. and S. Garc{\'\i}a-Burillo and Muller, S. and Winters, J.~M. and Gonzalez-Alfonso, E. and van der Werf, P. and Henkel, C. and F. Costagliola and Neri, R.} } @article {213, title = {{High-resolution imaging of the molecular outflows in two mergers: IRAS 17208-0014 and NGC 1614}}, journal = {Astronomy \& Astrophysics}, volume = {580}, year = {2015}, pages = {A35}, keywords = {galaxies: individual: IRAS 17208-0014, galaxies: individual: NGC1614, galaxies: ISM, galaxies: kinematics and dynamics, galaxies: nuclei, galaxies: starburst}, doi = {10.1051/0004-6361/201526133}, author = {Garcia-Burillo, S. and Combes, F. and Usero, A. and Aalto, S. and Colina, L. and Alonso-Herrero, A. and Hunt, L.~K. and Arribas, S. and Costagliola, F. and Labiano, A. and Neri, R. and Pereira-Santaella, M. and Tacconi, L.~J. and van der Werf, P.~P.} } @article {215, title = {{Probing highly obscured, self-absorbed galaxy nuclei with vibrationally excited HCN}}, journal = {ArXiv e-prints}, year = {2015}, keywords = {Astrophysics - Astrophysics of Galaxies}, author = {Aalto, S. and Costagliola, F. and Gonzalez-Alfonso, E. and Muller, S. and Sakamoto, K. and Fuller, G.~A. and Garcia-Burillo, S. and van der Werf, P. and Neri, R. and Spaans, M. and Combes, F. and Viti, S. and Muehle, S. and Armus, L. and Evans, A. and Sturm, E. and Cernicharo, J. and Henkel, C. and Greve, T.~R.} } @book {181, title = {{The Spanish Square Kilometre Array White Book}}, series = {ArXiv e-prints}, year = {2015}, keywords = {Astrophysics - Instrumentation and Methods for Astrophysics}, url = {http://adsabs.harvard.edu/abs/2015arXiv150603474A}, author = {Acosta-Pulido, J.~A. and Agudo, I. and Alberdi, A. and Alcolea, J. and Alfaro, E.~J. and Alonso-Herrero, A. and Anglada, G. and Arnalte-Mur, P. and Ascasibar, Y. and Ascaso, B. and Azulay, R. and Bachiller, R. and Baez-Rubio, A. and Battaner, E. and Blasco, J. and Brook, C.~B. and Bujarrabal, V. and Busquet, G. and Caballero-Garcia, M.~D. and Carrasco-Gonzalez, C. and Casares, J. and Castro-Tirado, A.~J. and Colina, L. and Colomer, F. and de Gregorio-Monsalvo, I. and del Olmo, A. and Desmurs, J.-F. and Diego, J.~M. and Dominguez-Tenreiro, R. and Estalella, R. and Fernandez-Soto, A. and Florido, E. and Font, J. and Font, J.~A. and Fuente, A. and Garc{\'\i}a-Benito, R. and Garcia-Burillo, S. and Garc{\'\i}a-Lorenzo, B. and Gil de Paz, A. and Girart, J.~M. and Goicoechea, J.~R. and G{\'o}mez, J.~F. and Gonzalez-Garcia, M. and Gonz{\'a}lez-Mart{\'\i}n, O. and Gonzalez-Serrano, J.~I. and Gorgas, J. and Gorosabel, J. and Guijarro, A. and Guirado, J.~C. and Hern{\'a}ndez-Garc{\'\i}a, L. and Hernandez-Monteagudo, C. and Herranz, D. and R. Herrero-Illana and Hu, Y.-D. and Huelamo, N. and Huertas-Company, M. and Iglesias-Paramo, J. and Jeong, S. and Jimenez-Serra, I. and Knapen, J.~H. and Lineros, R.~A. and Lisenfeld, U. and Marcaide, J.~M. and Marquez, I. and Marti, J. and Marti, J.~M. and Mart{\'\i}-Vidal, I. and Martinez-Gonzalez, E. and Martin-Pintado, J. and Masegosa, J. and Mayen-Gijon, J.~M. and Mezcua, M. and Migliari, S. and Mimica, P. and Mold{\'o}n, J. and Morata, O. and Negueruela, I. and Oates, S.~R. and Osorio, M. and Palau, A. and Paredes, J.~M. and Perea, J. and P{\'e}rez-Gonz{\'a}lez, P.~G. and Perez-Montero, E. and M. A. P{\'e}rez-Torres and Perucho, M. and Planelles, S. and Pons, J.~A. and Prieto, A. and Quilis, V. and Ramirez-Moreta, P. and Ramos Almeida, C. and Rea, N. and Rib{\'o}, M. and Rioja, M.~J. and Rodriguez Espinosa, J.~M. and Ros, E. and Rubi{\~n}o-Martin, J.~A. and Ruiz-Granados, B. and Sabater, J. and Sanchez, S. and Sanchez-Contreras, C. and Sanchez-Monge, A. and Sanchez-Ramirez, R. and Sintes, A.~M. and Solanes, J.~M. and Sopuerta, C.~F. and Tafalla, M. and Tello, J.~C. and Tercero, B. and Toribio, M.~C. and Torrelles, J.~M. and Torres, M.~A.~P. and Usero, A. and Verdes-Montenegro, L. and Vidal-Garcia, A. and Vielva, P. and Vilchez, J. and Zhang, B.-B.} } @article {232, title = {{Sub-arcsec mid-IR observations of NGC 1614: Nuclear star-formation or an intrinsically X-ray weak AGN?}}, journal = {ArXiv e-prints}, year = {2015}, keywords = {Astrophysics - Astrophysics of Galaxies}, url = {http://adsabs.harvard.edu/abs/2015arXiv150907765P}, author = {Pereira-Santaella, M. and Colina, L. and Alonso-Herrero, A. and Usero, A. and Diaz-Santos, T. and Garcia-Burillo, S. and Alberdi, A. and Gonz{\'a}lez-Mart{\'\i}n, O. and Herrero-Illana, R. and Imanishi, M. and Levenson, N.~A. and Perez-Torres, M.~A. and Ramos Almeida, C.} } @article {2014A\&A...565A..19R, title = {{The molecular gas content of ULIRG type 2 quasars at z {\l}t} 1}}, journal = {Astronomy and Astrophysics}, volume = {565}, year = {2014}, month = {may}, pages = {A19}, abstract = {We present new results of CO(1-0) spectroscopic observations of four Sloan Digital Sky Survey (SDSS) type 2 quasars (QSO2) at z \~{} 0.3, observed with the 30-m IRAM radio telescope. The QSO2 have infrared luminosities in the ultra-luminous infrared galaxies (ULIRG) regime. We confirm the CO(1-0) detection in one of our four QSO2, SDSS J1543-00, with L{\textquoteright}$_{CO}$ and M$_{H2}$ (1.2 {\plusmn} 0.2) {\times} 10$^{10}$ K km s$^{-1}$ pc$^{2}$ and (9.4 {\plusmn} 1.4) {\times} 10$^{9}$ M $_{\&sun;}$, respectively. The full width at half maximum (FWHM) of the CO(1-0) line is =575 {\plusmn} 102 km s$^{-1}$. No CO(1-0) emission is detected in SDSS J0903+02, SDSS J1337-01, SDSS J1520-01 above 3 sigma, yielding upper limits on M(H$_{2}$) \~{} 9.6, 4.3 and 5.1 {\times} 10$^{9}$ M$_{\&sun;}$, respectively. We expand previous studies of the molecular gas content of intermediate z QSO2 into the ULIRG regime. Taking into account nine QSO2 at z \~{} 0.3-1.0 from the literature, we discuss the location of the 13 ULIRG QSO2 at z {\l}t} 1 with available L{\textquoteright}$_{CO}$ measurements in the L{\textquoteright}$_{CO}$ vs. z and L{\textquoteright}$_{CO}$ vs. L$_{FIR}$ diagrams, in comparison with other QSO1 and ULIRG star forming samples. Based on observations carried out with the IRAM 30 m radiotelescope.}, keywords = {galaxies: ISM, quasars: emission lines, quasars: general}, doi = {10.1051/0004-6361/201323004}, url = {http://adsabs.harvard.edu/abs/2014A\%26A...565A..19R}, author = {M. Rodr{\'\i}guez and Villar-Mart{\'\i}n, M. and Emonts, B. and Humphrey, A. and Drouart, G. and S. Garc{\'\i}a-Burillo and P{\'e}rez Torres, M.} } @article {218, title = {{Molecular line emission in NGC 1068 imaged with ALMA. I. An AGN-driven outflow in the dense molecular gas}}, journal = {\aap}, volume = {567}, year = {2014}, pages = {A125}, keywords = {galaxies: individual: NGC 1068, galaxies: ISM, galaxies: kinematics and dynamics, galaxies: nuclei, galaxies: Seyfert, radio lines: galaxies}, doi = {10.1051/0004-6361/201423843}, author = {Garcia-Burillo, S. and Combes, F. and Usero, A. and Aalto, S. and Krips, M. and Viti, S. and Alonso-Herrero, A. and Hunt, L.~K. and Schinnerer, E. and Baker, A.~J. and Boone, F. and Casasola, V. and Colina, L. and Costagliola, F. and Eckart, A. and Fuente, A. and Henkel, C. and Labiano, A. and Mart{\'\i}n, S. and Marquez, I. and Muller, S. and Planesas, P. and Ramos Almeida, C. and Spaans, M. and Tacconi, L.~J. and van der Werf, P.~P.} } @article {2014A\&A...567A.125G, title = {{Molecular line emission in NGC 1068 imaged with ALMA. I. An AGN-driven outflow in the dense molecular gas}}, journal = {Astronomy and Astrophysics}, volume = {567}, year = {2014}, month = {jul}, pages = {A125}, abstract = {
Aims: We investigate the fueling and the feedback of star formation and nuclear activity in NGC 1068, a nearby (D = 14 Mpc) Seyfert 2 barred galaxy, by analyzing the distribution and kinematics of the molecular gas in the disk. We aim to understand if and how gas accretion can self-regulate.
Methods: We have used the Atacama Large Millimeter Array (ALMA) to map the emission of a set of dense molecular gas (n(H$_{2}$) {\sime} 10$^{5 - 6}$ cm$^{-3}$) tracers (CO(3-2), CO(6-5), HCN(4-3), HCO$^{+}$(4-3), and CS(7-6)) and their underlying continuum emission in the central r \~{} 2 kpc of NGC 1068 with spatial resolutions \~{}0.3{\Prime} - 0.5{\Prime} (\~{}20-35 pc for the assumed distance of D = 14 Mpc).
Results: The sensitivity and spatial resolution of ALMA give an unprecedented detailed view of the distribution and kinematics of the dense molecular gas (n(H$_{2}$) {\ge} 10$^{5 - 6}$cm$^{-3}$) in NGC 1068. Molecular line and dust continuum emissions are detected from a r \~{} 200 pc off-centered circumnuclear disk (CND), from the 2.6 kpc-diameter bar region, and from the r \~{} 1.3 kpc starburst (SB) ring. Most of the emission in HCO$^{+}$, HCN, and CS stems from the CND. Molecular line ratios show dramatic order-of-magnitude changes inside the CND that are correlated with the UV/X-ray illumination by the active galactic nucleus (AGN), betraying ongoing feedback. We used the dust continuum fluxes measured by ALMA together with NIR/MIR data to constrain the properties of the putative torus using CLUMPY models and found a torus radius of 20$^{+6}$$_{-10}$pc. The Fourier decomposition of the gas velocity field indicates that rotation is perturbed by an inward radial flow in the SB ring and the bar region. However, the gas kinematics from r \~{} 50 pc out to r \~{} 400 pc reveal a massive (M$_{mol}$\~{} 2.7$^{+0.9}$$_{-1.2}$ {\times} 10$^{7}$ M$_{\&sun;}$) outflow in all molecular tracers. The tight correlation between the ionized gas outflow, the radio jet, and the occurrence of outward motions in the disk suggests that the outflow is AGN driven.
Conclusions: The molecular outflow is likely launched when the ionization cone of the narrow line region sweeps the nuclear disk. The outflow rate estimated in the CND, dM/dt\~{} 63$^{+21}$$_{-37}$ M$_{\&sun;}$ yr$^{-1}$, is an order of magnitude higher than the star formation rate at these radii, confirming that the outflow is AGN driven. The power of the AGN is able to account for the estimated momentum and kinetic luminosity of the outflow. The CND mass load rate of the CND outflow implies a very short gas depletion timescale of {\l}e}1 Myr. The CND gas reservoir is likely replenished on longer timescales by efficient gas inflow from the outer disk. Based on observations carried out with ALMA in Cycle 0.}, keywords = {galaxies: individual: NGC 1068, galaxies: ISM, galaxies: kinematics and dynamics, galaxies: nuclei, galaxies: Seyfert, radio lines: galaxies}, doi = {10.1051/0004-6361/201423843}, url = {http://adsabs.harvard.edu/abs/2014A\%26A...567A.125G}, author = {S. Garc{\'\i}a-Burillo and Combes, F. and Usero, A. and Aalto, S. and Krips, M. and Viti, S. and Alonso-Herrero, A. and Hunt, L.~K. and Schinnerer, E. and Baker, A.~J. and Boone, F. and Casasola, V. and Colina, L. and F. Costagliola and Eckart, A. and Fuente, A. and Henkel, C. and Labiano, A. and Mart{\'\i}n, S. and Marquez, I. and Muller, S. and Planesas, P. and Ramos Almeida, C. and Spaans, M. and Tacconi, L.~J. and van der Werf, P.~P.} } @article {2014A\&A...570A..28V, title = {{Molecular line emission in NGC 1068 imaged with ALMA. II. The chemistry of the dense molecular gas}}, journal = {Astronomy and Astrophysics}, volume = {570}, year = {2014}, month = {oct}, pages = {A28}, abstract = {
Aims: We present a detailed analysis of Atacama Large Millimeter/submillimeter Array (ALMA) Bands 7 and 9 data of CO, HCO$^{+}$, HCN, and CS, augmented with Plateau de Bure Interferometer (PdBI) data of the \~{}200 pc circumnuclear disc (CND) and the \~{}1.3 kpc starburst ring (SB ring) of NGC 1068, a nearby (D = 14 Mpc) Seyfert 2 barred galaxy. We aim to determine the physical characteristics of the dense gas present in the CND, and to establish whether the different line intensity ratios we find within the CND, as well as between the CND and the SB ring, are due to excitation effects (gas density and temperature differences) or to a different chemistry.
Methods: We estimate the column densities of each species in local thermodynamic equilibrium (LTE). We then compute large one-dimensional, non-LTE radiative transfer grids (using RADEX) by using only the CO transitions first, and then all the available molecules to constrain the densities, temperatures, and column densities within the CND. We finally present a preliminary set of chemical models to determine the origin of the gas.
Results: We find that, in general, the gas in the CND is very dense ({\gt}10$^{5}$ cm$^{-3}$) and hot (T{\gt} 150 K), with differences especially in the temperature across the CND. The AGN position has the lowest CO/HCO$^{+}$, CO/HCN, and CO/CS column density ratios. The RADEX analyses seem to indicate that there is chemical differentiation across the CND. We also find differences between the chemistry of the SB ring and some regions of the CND; the SB ring is also much colder and less dense than the CND. Chemical modelling does not succeed in reproducing all the molecular ratios with one model per region, suggesting the presence of multi-gas phase components.
Conclusions: The LTE, RADEX, and chemical analyses all indicate that more than one gas-phase component is necessary to uniquely fit all the available molecular ratios within the CND. A higher number of molecular transitions at the ALMA resolution is necessary to determine quantitatively the physical and chemical characteristics of these components. Tables 5-11 are available in electronic form at http://www.aanda.org}, keywords = {galaxies: active, galaxies: individual: NGC 1068, galaxies: ISM, galaxies: nuclei, molecular processes, radio lines: galaxies}, doi = {10.1051/0004-6361/201424116}, url = {http://adsabs.harvard.edu/abs/2014A\%26A...570A..28V}, author = {Viti, S. and S. Garc{\'\i}a-Burillo and Fuente, A. and Hunt, L.~K. and Usero, A. and Henkel, C. and Eckart, A. and Mart{\'\i}n, S. and Spaans, M. and Muller, S. and Combes, F. and Krips, M. and Schinnerer, E. and Casasola, V. and F. Costagliola and Marquez, I. and Planesas, P. and van der Werf, P.~P. and Aalto, S. and Baker, A.~J. and Boone, F. and Tacconi, L.~J.} } @article {217, title = {{Molecular line emission in NGC 1068 imaged with ALMA. II. The chemistry of the dense molecular gas}}, journal = {\aap}, volume = {570}, year = {2014}, pages = {A28}, keywords = {galaxies: active, galaxies: individual: NGC 1068, galaxies: ISM, galaxies: nuclei, molecular processes, radio lines: galaxies}, doi = {10.1051/0004-6361/201424116}, author = {Viti, S. and Garcia-Burillo, S. and Fuente, A. and Hunt, L.~K. and Usero, A. and Henkel, C. and Eckart, A. and Mart{\'\i}n, S. and Spaans, M. and Muller, S. and Combes, F. and Krips, M. and Schinnerer, E. and Casasola, V. and Costagliola, F. and Marquez, I. and Planesas, P. and van der Werf, P.~P. and Aalto, S. and Baker, A.~J. and Boone, F. and Tacconi, L.~J.} } @article {2013MNRAS.434..978V, title = {{Molecular gas in type 2 quasars at z {\tilde} 0.2-0.3}}, journal = {Monthly Notices of the Royal Astronomical Society}, volume = {434}, year = {2013}, month = {sep}, pages = {978-991}, abstract = {{We present results of CO(1-0) spectroscopic observations of 10 Sloan Digital Sky Survey type 2 quasars (QSO2) at z {\tilde} 0.2-0.3 observed with the 30-m IRAM radio telescope and the Australia Telescope Compact Array. We report five new confirmed CO(1-0) detections and one tentative detection. They have L\^{}{\textquoteright} $\}$\_CO {\tilde} several {\times} 10$^{9}$ K km s$^{-1}$ pc$^{2}$, while upper limits for the non-detections are L\^{}{\textquoteright} $\}, keywords = {galaxies: evolution, galaxies: interactions, quasars: general}, author = {Villar-Mart{\'\i}n, M. and M. Rodr{\'\i}guez and Drouart, G. and Emonts, B. and Colina, L. and Humphrey, A. and S. Garc{\'\i}a-Burillo and Graci{\'a} Carpio, J. and Planesas, P. and P{\'e}rez Torres, M. and Arribas, S.} } @article {2012A\&A...537A..44A, title = {{Detection of HCN, HCO$^{+}$, and HNC in the Mrk 231 molecular outflow. Dense molecular gas in the AGN wind}}, journal = {Astronomy and Astrophysics}, volume = {537}, year = {2012}, month = {jan}, pages = {A44}, abstract = {
Aims: Our goal is to study gas properties in large-scale molecular outflows and winds from active galactic nuclei (AGNs) and starburst galaxies.
Methods: We obtained high-resolution (1.{\textquoteright}{\textquoteright}55 {\times} 1.{\textquoteright}{\textquoteright}28) observations of HCN, HCO$^{+}$, HNC 1-0 and HC$_{3}$N 10-9 of the ultraluminous galaxy (ULIRG) Mrk 231 with the IRAM Plateau de Bure Interferometer.
Results: We detect luminous emission from HCN, HCO$^{+}$ and HNC 1-0 in the QSO ULIRG Mrk 231. All three lines show broad line wings - which are particularly prominent for HCN. Velocities are found to be similar ( {\ap} {\plusmn} 750 km s$^{-1}$) to those found for CO 1-0. This is the first time bright HCN, HCO$^{+}$ and HNC emission has been detected in a large-scale galactic outflow. We find that both the blue- and red-shifted line wings are spatially extended by at least 0.{\textquoteright}{\textquoteright}75 ({\gt}700 pc) in a north-south direction. The line wings are brighter (relative to the line center intensity) in HCN than in CO 1-0 and line ratios suggest that the molecular outflow consists of dense (n {\gt} 10$^{4}$ cm$^{-3}$) and clumpy gas with a high HCN abundance X(HCN) {\gt} 10$^{-8}$. These properties are consistent with the molecular gas being compressed and fragmented by shocks in the outflow. Alternatively, HCN is instead pumped by mid-IR continuum, but we propose that this effect is not strong for the spatially extended outflowing gas. In addition, we find that the rotation of the main disk, in east-west direction, is also evident in the HCN, HCO$^{+}$ and HNC line emission. An unexpectedly bright HC$_{3}$N 10-9 line is detected inside the central 400 pc of Mrk 231. This HC$_{3}$N emission may emerge from a shielded, dust-enshrouded region within the inner 40-50 pc where the gas is heated to high temperatures (200-300 K) by the AGN. Based on observations carried out with the IRAM Plateau de Bure Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain).}, keywords = {galaxies: active, galaxies: evolution, galaxies: individual: Mrk 231, ISM: molecules, quasars: general, radio lines: ISM}, doi = {10.1051/0004-6361/201117919}, url = {http://adsabs.harvard.edu/abs/2012A\%26A...537A..44A}, author = {Aalto, S. and S. Garc{\'\i}a-Burillo and Muller, S. and Winters, J.~M. and van der Werf, P. and Henkel, C. and F. Costagliola and Neri, R.} }