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9 results on '"Mendes de Oliveira, C"'

1. Diagnostic diagrams for ram pressure stripped candidates.

Author

Krabbe, A C, Hernandez-Jimenez, J A, Mendes de Oliveira, C, Jaffe, Y L, Oliveira, C B, Cardoso, N M, Smith Castelli, A V, Dors, O L, Cortesi, A, and Crossett, J P

Subjects
IMAGE analysis, GALAXY clusters, GALACTIC evolution, UNIFIED modeling language, GALAXIES
Abstract

This paper presents a method for finding ram pressure stripped (RPS) galaxy candidates by performing a morphological analysis of galaxy images obtained from the Legacy survey. We consider a sample of about 600 galaxies located in different environments such as groups and clusters, tidally interacting pairs and the field. The sample includes 160 RPS previously classified in the literature into classes from J1 to J5, based on the increasing level of disturbances. Our morphological analysis was done using the astromorphlib software followed by the inspection of diagnostic diagrams involving combinations of different parameters like the asymmetry (A), concentration (C), Sérsic index (n), and bulge strength parameters |$F(G,\, M_{20})$|⁠. We found that some of those diagrams display a distinct region in which galaxies classified as J3, J4, and J5 decouples from isolated galaxies. We call this region as the morphological transition zone and we also found that tidally interacting galaxies in pairs are predominant within this zone. Nevertheless, after visually inspecting the objects in the morphological transition zone to discard obvious contaminants, we ended up with 33 bona fide new RPS candidates in the studied nearby groups and clusters (Hydra, Fornax, and CLoGS sample), of which one-third show clear evidence of unwinding arms. Future works may potentially further increase significantly the samples of known RPS using such method. [ABSTRACT FROM AUTHOR]

Published
2024
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2. The miniJPAS survey: A search for extreme emission-line galaxies

Author

Iglesias-Páramo, J., Arroyo-Polonio, A., Kehrig, C., Vílchez Medina, José Manuel, Duarte Puertas, Salvador, Pérez Montero, Enrique, Breda, I., Jiménez-Teja, Y., López Sanjuan, C., Lumbreras-Calle, A., Coelho, P., Gurung-López, S., Queiroz, C., Márquez, Isabel, Pović, Mirjana, González Delgado, Rosa M., Chaves-Montero, J., Sobral, D., Hernán-Caballero, A., Fernández-Ontiveros, J. A., Díaz-García, L. A., Alvarez-Candal, A., Abramo, R., Alcaniz, J., Benítez, Narciso, Bonoli, S., Cenarro, A. J., Cristóbal-Hornillos, D., Dupke, R., Ederoclite, A., Marín-Franch, A., Mendes de Oliveira, C., Moles, M., Sodré, L., Taylor, K., Varela, J., Vázquez-Ramió, H., J-PAS Team, Ministerio de Ciencia e Innovación (España), and European Commission

Subjects
Galaxies: star formation, Space and Planetary Science, Galaxies: evolution, Astronomy and Astrophysics, Galaxies: starburst, EVOLUÇÃO ESTELAR
Abstract

This is an Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited., Context. Galaxies with extreme emission lines (EELGs) may play a key role in the evolution of the Universe, as well as in our understanding of the star formation process itself. For this reason an accurate determination of their spatial density and fundamental properties in different epochs of the Universe will constitute a unique perspective towards a comprehensive picture of the interplay between star formation and mass assembly in galaxies. In addition to this, EELGs are also interesting in order to explain the reionization of the Universe, since their interstellar medium (ISM) could be leaking ionizing photons, and thus they could be low z, analogous of extreme galaxies at high z. Aims. This paper presents a method to obtain a census of EELGs over a large area of the sky by detecting galaxies with rest-frame equivalent widths ≥300 Å in the emission lines [O II]λλ3727,3729Å, [O III]λ5007Å, and Hα. For this, we aim to use the J-PAS survey, which will image an area of ≈8000 deg2 with 56 narrow band filters in the optical. As a pilot study, we present a methodology designed to select EELGs on the miniJPAS images, which use the same filter dataset as J-PAS, and thus will be exportable to this larger survey. Methods. We make use of the miniJPAS survey data, conceived as a proof of concept of J-PAS, and covering an area of ≈1 deg2. Objects were detected in the rSDSS images and selected by imposing a condition on the flux in a given narrow-band J-PAS filter with respect to the contiguous ones, which is analogous to requiring an observed equivalent width larger than 300 Å in a certain emission line within the filter bandwidth. The selected sources were then classified as galaxies or quasi-stellar objects (QSOs) after a comparison of their miniJPAS fluxes with those of a spectral database of objects known to present strong emission lines. This comparison also provided a redshift for each source, which turned out to be consistent with the spectroscopic redshifts when available (|Δz/(1 + zspec)| ≤ 0.01). Results. The selected candidates were found to show a compact appearance in the optical images, some of them even being classified as point-like sources according to their stellarity index. After discarding sources classified as QSOs, a total of 17 sources turned out to exhibit EW0 ≥ 300 Å in at least one emission line, thus constituting our final list of EELGs. Our counts are fairly consistent with those of other samples of EELGs in the literature, although there are some differences, which were expected due to biases resulting from different selection criteria. © J. Iglesias-Páramo et al. 2022., This work has been partially funded by projects PID2019-107408GB-C44 from the Spanish PNAYA, co-funded with FEDER, and grand P18-FR-2664, funded by Junta de Andalucía. We acknowledge financial support from the State Agency for Research of the Spanish MCIU through the “Center of Excellence Severo Ochoa” award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). RGD and LADG acknowledge financial support from the State Agency for Research of the Spanish MCIU through the “Center of Excellence Severo Ochoa” award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709), and PID2019-109067-GB100. IM acknowledges financial support from the State Agency for Research of the Spanish MCIU through the PID2019-106027GB-C41. JCM acknowledges partial support from the Spanish Ministry of Science, Innovation and Universities (MCIU/AEI/FEDER, UE) through the grant PGC2018-097585-B-C22. SDP is grateful to the Fonds de Recherche du Québec – Nature et Technologies. LSJ acknowledges the support of CNPq (304819/2017-4) and FAPESP (2019/10923-5). JAFO acknowledges the financial support from the Spanish Ministry of Science and Innovation and the European Union – NextGenerationEU through the Recovery and Resilience Facility project ICTS-MRR-2021-03- CEFCA. Funding for the J-PAS Project has been provided by the Governments of España and Aragón though the Fondo de Inversión de Teruel, European FEDER funding and the MINECO and by the Brazilian agencies FINEP, FAPESP, FAPERJ and by the National Observatory of Brazil. Based on observations made with the JST/T250 telescope and PathFinder camera for the miniJPAS project at the Observatorio Astrofísico de Javalambre (OAJ), in Teruel, owned, managed, and operated by the Centro de Estudios de Física del Cosmos de Aragón (CEFCA). We acknowledge the OAJ Data Processing and Archiving Unit (UPAD) for reducing and calibrating the OAJ data used in this work. Funding for OAJ, UPAD, and CEFCA has been provided by the Governments of Spain and Aragón through the Fondo de Inversiones de Teruel; the Aragón Government through the Research Groups E96, E103, and E16_17R; the Spanish Ministry of Science, Innovation and Universities (MCIU/AEI/FEDER, UE) with grant PGC2018-097585-B-C21; the Spanish Ministry of Economy and Competitiveness (MINECO/FEDER, UE) under AYA2015-66211-C2-1-P, AYA2015-66211-C2-2, AYA2012-30789, and ICTS-2009-14; and European FEDER funding (FCDD10-4E-867, FCDD13-4E-2685). This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Funding for SDSS-IV has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-IV web site is https://www.sdss.org/. This project has received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No 898633.

Published
2022

3. The miniJPAS Survey: Detection of the double-core Lyα morphology for two high-redshift QSOs

Author

Rahna, P. T., Zheng, Zhen-Ya, Chies-Santos, A. L., Cai, Z. Y., Spinoso, Daniele, Márquez, Isabel, Overzier, Roderik, Abramo, L. R., Bonoli, S., Kehrig, C., Díaz-García, L. A., Pović, Mirjana, Soria, R., Diego, José María, Broadhurst, Tom, González Delgado, Rosa M., Alcaniz, J., Benítez, Narciso, Carneiro, Saulo, Cenarro, A. J., Cristóbal-Hornillos, David, Dupke, R. A., Ederoclite, Alessandro, Hernán-Caballero, Antonio, López-Sanjuan, C., Marín-Franch, Antonio, Mendes de Oliveira, C., Moles, Mariano, Sodré Jr., L., Taylor, K., Varela, Jesús, Vázquez Ramió, H., JPAS team, National Science Foundation (US), Pioneer Fund, Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Fundação de Amparo à Pesquisa do Estado do Rio Grande do Sul, Chinese Academy of Sciences, Japan Society for the Promotion of Science, Japan Science and Technology Agency, Gobierno de Aragón, European Commission, Fondo de Inversiones de Teruel, Ministerio de Ciencia, Innovación y Universidades (España), National Natural Science Foundation of China, Fundações de Amparo à Pesquisa (Brasil), University of Tartu, Agencia Estatal de Investigación (España), and National Astronomical Observatory of China

Subjects
Quasars: general, Quasars: emission lines, Space and Planetary Science, Galaxies: high-redshift, Galaxies: evolution, Astronomy and Astrophysics, Galaxies: formation, Intergalactic medium
Abstract

Extragalactic astronomy., [Context] The Lyα emission is an important tracer of neutral gas in a circum-galactic medium (CGM) around high-z quasi-stellar objects (QSOs). The origin of Lyα emission around QSOs is still under debate, bringing on significant implications for galaxy formation and evolution., [Aims] In this paper, we study Lyα nebulae around two high redshift QSOs, SDSS J141935.58+525710.7 at z = 3.218 (hereafter QSO1) and SDSS J141813.40+525240.4 at z = 3.287 (hereafter QSO2), from the miniJPAS survey within the All-wavelength Extended Groth Strip International Survey (AEGIS) field., [Methods] Using the contiguous narrow-band (NB) images from the miniJPAS survey and Sloan Digital Sky Survey (SDSS) spectra, we analyzed their morphology, nature, and origin., [Results] We report the serendipitous detection of double-core Lyα morphology around two QSOs, which is rarely seen among other QSOs. The separations of the two Lyα cores are 11.07 ± 2.26 kpcs (1.47 ± 0.3″) and 9.73 ± 1.55 kpcs (1.31 ± 0.21″), with Lyα line luminosities of ∼3.35 × 1044 erg s−1 and ∼6.99 × 1044 erg s −1 for QSO1 and QSO2, respectively. The miniJPAS NB images show evidence of extended Lyα and CIV morphology for both QSOs and extended HeII morphology for QSO1., [Conclusions] These two QSOs may be potential candidates for the new enormous Lyman alpha nebula (ELAN) found from the miniJPAS survey due to their extended morphology in the shallow depth and relatively high Lyα luminosities. We suggest that galactic outflows are the major powering mechanism for the double-core Lyα morphology. Considering the relatively shallow exposures of miniJPAS, the objects found here could merely form the cusp of a promising number of such objects that will be uncovered in the upcoming full Javalambre-Physics of the Accelerated Universe Astrophysical Survey (J-PAS) survey and deep integral field units (IFU) observations with 8–10 m telescopes will be essential for constraining the underlying physical mechanism that is responsible for the double-cored morphology., Z.Y.Z. acknowledges support by the National Science Foundation of China (12022303), the China-Chile Joint Research Fund (CCJRF No. 1906), and the CAS Pioneer Hundred Talents Program. RPT thanks the CAS President’s International Fellowship Initiative (PIFI) (Grant No. E085201009) for supporting this work. We acknowledge the science research grants from the China Manned Space Project with No. CMS-CSST-2021-A04 and CMS-CSST-2021-A07. ACS acknowledges funding from the Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq) and the Rio Grande do Sul Research Foundation (FAPERGS) through grants CNPq-11153/2018-6, CNPq-314301/2021-6 and FAPERGS/CAPES 19/2551-0000696-9 and the Chinese Academy of Sciences (CAS) President’s International Fellowship Initiative (PIFI) through grant E085201009. R.P.T. and Z.Y.Z. thanks Shuairu Zhu, Fang-Ting Yuan, Ruqiu Lin, and Xiang Ji for their useful discussion during the preparations of the manuscript. R.P.T. acknowledges Carolina Queiroz for sharing information about the JPAS database. This paper has gone through the internal review by the J-PAS collaboration. Based on observations made with the JST/T250 telescope and JP Cam at the Observatorio Astrofísico de Javalambre (OAJ), in Teruel, owned, managed, and operated by the Centro de Estudios de Física del Cosmos de Aragón (CEFCA). We acknowledge the OAJ Data Processing and Archiving Unit (UPAD) for reducing and calibrating the OAJ data used in this work. Funding for the J-PAS Project has been provided by the Governments of Spain and Aragón through the Fondo de Inversión de Teruel, European FEDER funding and the Spanish Ministry of Science, Innovation and Universities, and by the Brazilian agencies FINEP, FAPESP, FAPERJ and by the National Observatory of Brazil. Additional funding was also provided by the Tartu Observatory and by the J-PAS Chinese Astronomical Consortium. L.A.D.G., C.K., and R.G.D., acknowledge financial support from the State Agency for Research of the Spanish MCIU through the “Center of Excellence Severo Ochoa” award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709), and to PID2019-109067-GB100.

Published
2022

4. Physical and kinematic conditions of the local merging galaxy NGC 1487.

Author

Buzzo, M L, Ziegler, B, Amram, P, Verdugo, M, Barbosa, C E, Ciocan, B, Papaderos, P, Torres-Flores, S, and Mendes de Oliveira, C

Subjects
INTEGRAL field spectroscopy, DWARF galaxies, GALAXY clusters, PHYSICAL training & conditioning, IONIZED gases, SOLAR radio bursts
Abstract

We present optical VLT/MUSE integral field spectroscopy data of the merging galaxy NGC 1487. We use fitting techniques to study the ionized gas emission of this merger and its main morphological and kinematical properties. We measured flat and sometimes inverted oxygen abundance gradients in the subsystems composing NGC 1487, explained by metal mixing processes common in merging galaxies. We also measured widespread star-forming bursts, indicating that photoionization by stars is the primary ionization source of the galaxy. The kinematic map revealed a rotating pattern in the gas in the northern tail of the system, suggesting that the galaxy may be in the process of rebuilding a disc. The gas located in the central region has larger velocity dispersion (σ ≈ 50 km s−1) than the remaining regions, indicating kinematic heating, possibly owing to the ongoing interaction. Similar trends were, however, not observed in the stellar velocity dispersion map, indicating that the galaxy has not yet achieved equilibrium, and the nebular and stellar components are still kinematically decoupled. Based on all our measurements and findings, and specially on the mass estimates, metallicity gradients, and velocity fields of the system, we propose that NGC 1487 is the result of an ongoing merger event involving smallish dwarf galaxies within a group, in a pre-merger phase, resulting in a relic with mass and physical parameters similar to a dwarf galaxy. Thus, we may be witnessing the formation of a dwarf galaxy by merging of smaller clumps at z = 0. [ABSTRACT FROM AUTHOR]

Published
2021
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5. The Hα kinematics of interacting galaxies in 12 compact groups★.

Author

Torres-Flores, S., Amram, P., Mendes de Oliveira, C., Plana, H., Balkowski, C., Marcelin, M., and Olave-Rojas, D.

Subjects
ASTRONOMICAL observations, GALACTIC evolution, KINEMATICS, COMPACT groups, MONOCHROMATIC light, FABRY-Perot resonators, GALACTIC dynamics
Abstract

We present new Fabry-Perot observations for a sample of 42 galaxies located in 12 compact groups of galaxies: HCG 1, HCG 14, HCG 25, HCG 44, HCG 53, HCG 57, HCG 61, HCG 69, HCG 93, VV 304, LGG 455 and Arp 314. From the 42 observed galaxies, a total of 26 objects are spiral galaxies, which range from Sa to Im morphological types. The remaining 16 objects are E, S0 and S0a galaxies. Using these observations, we have derived velocity maps, monochromatic and velocity dispersion maps for 24 galaxies, where 18 are spiral, three are S0a, two are S0 and one is an Im galaxy. From the 24 velocity fields obtained, we could derive rotation curves for 15 galaxies; only two of them exhibit rotation curves without any clear signature of interactions. Based on kinematic information, we have evaluated the evolutionary stage of the different groups of the current sample. We identify groups that range from having no Hα emission to displaying an extremely complex kinematics, where their members display strongly perturbed velocity fields and rotation curves. In the case of galaxies with no Hα emission, we suggest that past galaxy interactions removed their gaseous components, thereby quenching their star formation. However, we cannot discard that the lack of Hα emission is linked with the detection limit for some of our observations. [ABSTRACT FROM AUTHOR]

Published
2014
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6. Intragroup diffuse light in compact groups of galaxies – II. HCG 15, 35 and 51.

Author

Da Rocha, C., Ziegler, B. L., and Mendes de Oliveira, C.

Subjects
GALAXY clusters, DARK matter, STELLAR luminosity function, GRAVITATIONAL potential, WAVELETS (Mathematics), ASTRONOMICAL photometry
Abstract

This continuing study of intragroup light in compact groups of galaxies aims to establish new constraints to models of formation and evolution of galaxy groups, specially of compact groups, which are a key part in the evolution of larger structures, such as clusters. In this paper we present three additional groups (HCG 15, 35 and 51) using deep wide-field B- and R-band images observed with the LAICA camera at the 3.5-m telescope at the Calar Alto observatory (CAHA). This instrument provides us with very stable flat-fielding, a mandatory condition for reliably measuring intragroup diffuse light. The images were analysed with theov_wav package, a wavelet technique that allows us to uncover the intragroup component in an unprecedented way. We have detected that 19, 15 and 26 per cent of the total light of HCG 15, 35 and 51, respectively, are in the diffuse component, with colours that are compatible with old stellar populations and with mean surface brightness that can be as low as 28.4 B mag arcsec−2. Dynamical masses, crossing times and mass-to-light ratios were recalculated using the new group parameters. Also tidal features were analysed using the wavelet technique. [ABSTRACT FROM AUTHOR]

Published
2008
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7. The Munich Near-Infrared Cluster Survey – I. Field selection, object extraction and photometry.

Author

Drory, N., Feulner, G., Bender, R., Botzler, C.S., Hopp, U., Maraston, C., Mendes de Oliveira, C., and Snigula, J.

Subjects
GALAXIES, SCIENTIFIC surveys, ASTRONOMICAL photometry
Abstract

The Munich Near-Infrared Cluster Survey (MUNICS) is a wide-area, medium-deep, photometric survey selected in the K′ band. It covers an area of roughly 1 deg[sup 2] in the K′ and J near-IR passbands. The survey area consists of 16 6×6 arcmin[sup 2] fields targeted at QSOs with redshifts 0.5

Published
2001
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8. The co-responsibility of mass and environment in the formation of lenticular galaxies.

Author

Cortesi, A., Coccato, L., Buzzo, M. L., Menéndez-Delmestre, K., Goncalves, T., Mendes de Oliveira, C., Merrifield, M., Arnaboldi, M., Bergmann, Thaisa Storchi, Forman, William, Overzier, Roderik, and Riffel, Rogério

Abstract

We present the latest data release of the Planetary Nebulae Spectrograph Survey (PNS) of ten lenticular galaxies and two spiral galaxies. With this data set we are able to recover the galaxies' kinematics out to several effective radii. We use a maximum likelihood method to decompose the disk and spheroid kinematics and we compare it with the kinematics of spiral and elliptical galaxies. We build the Tully- Fisher (TF) relation for these galaxies and we compare with data from the literature and simulations. We find that the disks of lenticular galaxies are hotter than the disks of spiral galaxies at low redshifts, but still dominated by rotation velocity. The mechanism responsible for the formation of these lenticular galaxies is neither major mergers, nor a gentle quenching driven by stripping or Active Galactic Nuclei (AGN) feedback. [ABSTRACT FROM AUTHOR]

Published
2019
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9. A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE).IV. A tail of Ionised Gas in the Merger Remnant NGC 4424

Author

P. Cote, Laura Ferrarese, Hanindyo Kuncarayakti, P. Amram, Jean-Charles Cuillandre, V. Buat, Gerhard Hensler, Benoît Epinat, Médéric Boquien, J. Roediger, Elisa Toloba, G. Consolandi, Patrick R. Durrell, Rubén Sánchez-Janssen, Matteo Fossati, Luca Cortese, Ginevra Trinchieri, Lluís Galbany, Sebastián F. Sánchez, Samuel Boissier, Joseph P. Anderson, M. Marcelin, J. A. Gómez-López, S. D. J. Gwyn, Denis Burgarella, Michele Fumagalli, Chong Ge, B. Vollmer, Y. Roehlly, Giuseppe Gavazzi, Alessandro Boselli, C. Mendes de Oliveira, Ming Sun, Bruno Quint, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Milano-Bicocca [Milano] (UNIMIB), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Ingénierie des Matériaux Polymères (IMP), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet [Saint-Étienne] (UJM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Uppsala University, European Synchrotron Radiation Facility (ESRF), Centre de Recherche en Paléontologie - Paris (CR2P), Muséum national d'Histoire naturelle (MNHN)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Service d'Oncologie Médicale [CHRU Besançon], Centre Hospitalier Régional Universitaire de Besançon (CHRU Besançon)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB), Youngstown State University (YSU), NRC Herzberg Astronomy and Astrophysics, Conseil National de Recherches Canada (CNRC), University of Vienna [Vienna], UCO/Lick Observatory, University of California [Santa Cruz] (UC Santa Cruz), University of California (UC)-University of California (UC), CDS, Centre de Données astronomiques de Strasbourg, Observatoire astronomique de Strasbourg, France + ESO, European Southern Observatory, Garching bei Muenchen, Allemagne, Université de Strasbourg (UNISTRA)-Université Louis Pasteur - Strasbourg I, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet - Saint-Étienne (UJM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), University of California [Santa Cruz] (UCSC), University of California-University of California, Boselli, A, Fossati, M, Consolandi, G, Amram, P, Ge, C, Sun, M, Anderson, J, Boissier, S, Boquien, M, Buat, V, Burgarella, D, Cortese, L, Cote, P, Cuillandre, J, Durrell, P, Epinat, B, Ferrarese, L, Fumagalli, M, Galbany, L, Gavazzi, G, Gomez-Lopez, J, Gwyn, S, Hensler, G, Kuncarayakti, H, Marcelin, M, Mendes De Oliveira, C, Quint, B, Roediger, J, Roehlly, Y, Sanchez, S, Sanchez-Janssen, R, Toloba, E, Trinchieri, G, Vollmer, B, ITA, USA, GBR, FRA, DEU, AUS, CAN, and CHL

Subjects
Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Peculiar galaxy, Intracluster medium, 0103 physical sciences, Galaxy formation and evolution, galaxies: interactions, Astrophysics::Solar and Stellar Astrophysics, Surface brightness, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, GALÁXIAS, Virgo Cluster, Astrophysics - Astrophysics of Galaxies, Galaxy, Ram pressure, Galaxies: interaction, 13. Climate action, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), galaxies: clusters: individual: Virgo, galaxies: individual: NGC 4424, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM
Abstract

We have observed the late-type peculiar galaxy NGC 4424 during VESTIGE, a blind narrow-band Halpha[NII] imaging survey of the Virgo cluster carried out with MegaCam at the CFHT. The presence of a 110 kpc long HI tail in the S direction indicates that this galaxy is undergoing a ram pressure stripping event. The deep narrow-band image revealed the presence of a low surface brightness ionised gas tail ~10 kpc long extending from the centre of the galaxy to the NW direction, in the direction opposite to the HI tail. Chandra and XMM X-rays data do not show any compact source in the nucleus nor the presence of an extended tail of hot gas, while MUSE spectroscopy indicates that the gas is photo-ionised in the inner regions and shock-ionised in the outer parts. IFU spectroscopy confirms that the ionised gas is kinematically decoupled from the stellar component and indicates the presence of two kinematically distinct structures in the stellar disc. The analysis of the SED of the galaxy indicates that the activity of star formation has been totally quenched in the outer disc ~ 250-280 Myr ago, while only reduced by ~80% in the central regions. All this observational evidence suggests that NGC 4424 is the remnant of an unequal-mass merger occurred, Accepted for publication on Astronomy & Astrophysics

Published
2018

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