A proto-pseudobulge in ESO 320-G030 fed by a massive molecular inflow driven by a nuclear bar

Autor: Sara Cazzoli, Eduardo González-Alfonso, Fernando Rico-Villas, Matthew L. N. Ashby, C. Yang, K. P. Stewart, Luis Colina, Howard A. Smith, Jesús Martín-Pintado, Almudena Alonso-Herrero, Jacqueline Fischer, Miguel Pereira-Santaella, Santiago García-Burillo
Přispěvatelé: Ministerio de Economía y Competitividad (España), National Aeronautics and Space Administration (US), Comunidad de Madrid, Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Agencia Estatal de Investigación (España), Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, National Aeronautics and Space Administration (NASA), Agencia Estatal de Investigación (AEI), European Commission (EC), González Alfonso, E. [0000-0001-5285-8517], Fischer, J. [0000-0001-6697-7808], García Burillo, S. [0000-0003-0444-6897], Yang, C. [0000-0002-8117-9991], Alonso Herrero, A. [0000-0001-6794-2519], Cazzoli, S. [0000-0002-7705-2525], Stewart, K. P. [0000-0001-8266-8298], ESO Telescopes at the Paranal Observatory, ID 086.B-0901(A), Spanish Ministerio de Economia y Competitividad, ESP2017-86582-C4-1-R and PID2019-105552RB-C41 ESP2017-83197, Centro de Excelencia Científica Severo Ochoa Instituto de Astrofísica de Andalucía del CSIC, SEV-2017-0709
Jazyk: angličtina
Rok vydání: 2021
Předmět:
Zdroj: Digital.CSIC. Repositorio Institucional del CSIC
instname
DIGITAL.INTA Repositorio Digital del Instituto Nacional de Técnica Aeroespacial
Instituto Nacional de Técnica Aeroespacial (INTA)
Popis: Galaxies with nuclear bars are believed to efficiently drive gas inward, generating a nuclear starburst and possibly an active galactic nucleus. We confirm this scenario for the isolated, double-barred, luminous infrared galaxy ESO 320-G030 based on an analysis of Herschel and ALMA spectroscopic observations. Herschel/PACS and SPIRE observations of ESO 320-G030 show absorption or emission in 18 lines of H2O, which we combine with the ALMA H2O 4(23)-3(30) 448 GHz line (E-upper similar to 400 K) and continuum images to study the physical properties of the nuclear region. Radiative transfer models indicate that three nuclear components are required to account for the multi-transition H2O and continuum data. An envelope, with radius R similar to 130-150 pc, dust temperature T-dust approximate to 50 K, and N-H2 similar to 2x10(23) cm(-2), surrounds a nuclear disk with R similar to 40 pc that is optically thick in the far-infrared (tau (100 mu m)similar to 1.5-3, N-H2 similar to 2x10(24) cm(-2)). In addition, an extremely compact (R similar to 12 pc), warm (approximate to 100 K), and buried (tau (100 mu m)> 5, N-H2 greater than or similar to 5x10(24) cm(-2)) core component is required to account for the very high-lying H2O absorption lines. The three nuclear components account for 70% of the galaxy luminosity (SFR similar to 16-18 M-circle dot yr(-1)). The nucleus is fed by a molecular inflow observed in CO 2-1 with ALMA, which is associated with the nuclear bar. With decreasing radius (r=450-225 pc), the mass inflow rate increases up to M-inf similar to 20 M yr(-1), which is similar to the nuclear star formation rate (SFR), indicating that the starburst is sustained by the inflow. At lower r, similar to 100-150 pc, the inflow is best probed by the far-infrared OH ground-state doublets, with an estimated M-inf similar to 30 M yr(-1). The inferred short timescale of similar to 20 Myr for nuclear gas replenishment indicates quick secular evolution, and indicates that we are witnessing an intermediate stage (< 100 Myr) proto-pseudobulge fed by a massive inflow that is driven by a strong nuclear bar. We also apply the H2O model to the Herschel far-infrared spectroscopic observations of H218O, OH, 18OH, OH+, H2O+, H3O+, NH, NH2, NH3, CH, CH+, 13CH+, HF, SH, and C3, and we estimate their abundances. © ESO 2021.
EG-A is grateful for the warm hospitality of the Harvard-Smithsonian Center for Astrophysics, where part of the present study was carried out, and thanks Javier Goicoechea for useful conversations on the far-IR spectrum of Sgr B2, Alex Crespo Gomez for sharing preliminary results on the stellar kinematics in ESO 320-G030, and Juan Rafael Martinez-Galarza for useful conversations on the Bayesian analysis. We thank the anonymous referee for constructive and helpful comments on the manuscript. PACS was developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAFIFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). SPIRE was developed by a consortium of institutes led by Cardiff University (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); and Caltech, JPL, NHSC, Univ.Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA). This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.1.00263.S and ADS/JAO.ALMA#2013.1.00271.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) and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. Based on observations made with ESO Telescopes at the Paranal Observatory under programme ID 086.B-0901(A). EG-A is a Research Associate at the Harvard-Smithsonian Center for Astrophysics. EG-A, JM-P, and FR-V thank the Spanish Ministerio de Economia y Competitividad for support under projects ESP2017-86582-C4-1-R and PID2019-105552RB-C41. EG-A and HAS thank NASA grant ADAP NNX15AE56G. MP-S acknowledges support from the Comunidad de Madrid, Spain, through Atraccion de Talento Investigador Grant 2018-T1/TIC-11035 and PID2019-105423GA-I00 (MCIU/AEI/FEDER,UE). AA-H and SG-B acknowledge support through grant PGC2018-094671-B-I00 (MCIU/AEI/FEDER,UE). LC, AA-H, MP-S, and JM-P acknowledge support under project No. MDM-2017-0737 Unidad de Excelencia "Maria de Maeztu" - Centro de Astrobiologia (INTA-CSIC). SG-B acknowledges support from the Spanish MINECO and FEDER funding grant AYA2016-76682-C3-2-P. C.Y. acknowledges support from an ESO Fellowship. LC acknowledges support from the Spanish Ministerio de Economia y Competitividad for support under project ESP2017-83197. SC acknowledges financial support from the State Agency for Research of the Spanish MCIU through the 'Center of Excellence Severo Ochoa' award to the Instituto de Astrofisica de Andalucia (SEV-2017-0709). This research has made use of NASA's Astrophysics Data System (ADS) and of GILDAS software.
Databáze: OpenAIRE
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