SUPER V. ALMA continuum observations of z~2 AGN and the elusive evidence of outflows influencing star formation
I. Lamperti, C. M. Harrison, V. Mainieri, D. Kakkad, M. Perna, C. Circosta, J. Scholtz, S. Carniani, C. Cicone, D. M. Alexander, M. Bischetti, G. Calistro River… 展开作者
I. Lamperti, C. M. Harrison, V. Mainieri, D. Kakkad, M. Perna, C. Circosta, J. Scholtz, S. Carniani, C. Cicone, D. M. Alexander, M. Bischetti, G. Calistro Rivera, C. -C. Chen, G. Cresci, C. Feruglio, F. Fiore, F. Mannucci, A. Marconi, L. N. Martínez-Ramírez, H. Netzer, E. Piconcelli, A. Puglisi, D. J. Rosario, M. Schramm, G. Vietri, C. Vignali, L. Zappacosta
We study the impact of AGN ionised outflows on star formation in high-redshift AGN hosts, by combining NIR IFS observations, mapping the H$α$ emission and [OIII] outflows, with matched-resolution observations of the rest-frame FIR emission. We present high-resolution ALMA Band 7 observations of eight X-ray selected AGN at z~2 from the SUPER sample, targeting the rest-frame ~260 um continuum at ~2 kpc (0.2'') resolution. We detected 6 out of 8 targets with S/N>10 in the ALMA maps, with continuum flux densities F = 0.27-2.58 mJy and FIR half-light radii Re = 0.8-2.1 kpc. The FIR Re of our sample are comparable to other AGN and star-forming galaxies at a similar redshift from the literature. However, we find that the mean FIR size in X-ray AGN (Re = 1.16+/- 0.11 kpc) is slightly smaller than in non-AGN (Re = 1.69+/-0.13 kpc). From SED fitting, we find that the main contribution to the 260 um flux density is dust heated by star formation, with < 4% contribution from AGN-heated dust and < 1% from synchrotron emission. The majority of our sample show different morphologies for the FIR (mostly due to reprocessed stellar emission) and the ionised gas emission (H$α$ and [OIII], mostly due to AGN emission). This could be due to the different locations of dust and ionised gas, the different sources of the emission (stars and AGN), or the effect of dust obscuration. We are unable to identify any residual H$α$ emission, above that dominated by AGN, that could be attributed to star formation. Under the assumption that the FIR emission is a reliable tracer of obscured star formation, we find that the obscured star formation activity in these AGN host galaxies is not clearly affected by the ionised outflows. However, we cannot rule out that star formation suppression is happening on smaller spatial scales than the ones we probe with our observations (< 2 kpc) or on different timescales.
Elusive helium stars in the gap between subdwarfs and Wolf-Rayet stars III. Formation of the Galactic population of stripped helium stars
Institute of Astronomy, Russian Academy of Sciences（俄罗斯科学院天文研究所）；Sternberg Astronomical Institute, M.V. Lomonosov Moscow State University（莫斯科国立大学谢尔盖·斯特恩伯格天文研究所）；Moscow Institute of Physics and Technology（莫斯科物理技术学院）
ALMA Chemical Evolution (ACE) survey: the dust content of subsolar metallicity galaxies at cosmic noon
Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心）；European Southern Observatory（欧洲南方天文台）；Leiden Observatory, Leiden University（莱顿大学天文台）；Department of Astronomy, University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校天文学系）；Departamento de Física de la Tierra y Astrofísica, Facultad de Ciencias Físicas, Universidad Complutense de Madrid（马德里康普顿斯大学物理科学学院地球与天体物理学系）；Department of Physics and Astronomy, University of California, Riverside（加州大学河滨分校物理与天文学系）；Department of Astronomy, University of Florida（佛罗里达大学天文学系）
The 10-15 GHz radio continuum survey of the Galactic Plane with SKAO
West Virginia University（西弗吉尼亚大学）；University of Geneva（日内瓦大学）；Korea Astronomy and Space Science Institute (KASI)（韩国天体宇宙科学研究所）；Tata Institute of Fundamental Research（塔塔基础研究所）；Royal Observatory Edinburgh（爱丁堡皇家天文台）；National Astronomical Observatory of Japan（日本国立天文台）；Indian Institute of Space Science and Technology (IIST)（印度空间科学与技术学院）；Université Paris-Saclay（巴黎萨克雷大学）；University of Leeds（利兹大学）；University of Manchester（曼彻斯特大学）；University of Kent（肯特大学）；Univ. Bordeaux（波尔多大学）；Univ. Grenoble Alpes（格勒诺布尔阿尔卑斯大学）；Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；Aix Marseille Univ（艾克斯-马赛大学）；Sorbonne Université（索邦大学）；Observatoire de Paris（巴黎天文台）；University of Central Florida（中佛罗里达大学）；University of Puerto Rico（波多黎各大学）；Nicolaus Copernicus University in Toruń（托伦哥白尼大学）；Chinese Academy of Sciences（中国科学院）；Rhodes University（罗德斯大学）；University of Vienna（维也纳大学）；Chalmers University of Technology（查尔姆斯理工大学）；Peking University（北京大学）
The efficient star-forming regions of stripped-envelope supernovae
Adam Mickiewicz University（亚当·密茨凯维奇大学）；Astronomical Observatory Institute, Faculty of Physics and Astronomy, Adam Mickiewicz University（亚当·密茨凯维奇大学物理与天文学学院天文台研究所）；Instituto de Astrofísica de Canarias（加那利群岛天体物理学研究所）；Universidad de La Laguna (ULL)（拉帕尔马大学）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所（ICE，CSIC））；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚太空研究研究所（IEEC））；European Southern Observatory（欧洲南方天文台）；The Oskar Klein Centre, Department of Astronomy, Stockholm University（斯德哥尔摩大学奥谢·克莱因中心天文学系）；National and Kapodistrian University of Athens（雅典国家卡波季斯特里安大学）；Institute of Astrophysics, Foundation for Research a
