TY - JOUR
T1 - XXL-HSC
T2 - Link between AGN activity and star formation in the early Universe (z ≥ 3.5)
AU - Pouliasis, E.
AU - Mountrichas, G.
AU - Georgantopoulos, I.
AU - Ruiz, A.
AU - Gilli, R.
AU - Koulouridis, E.
AU - Akiyama, M.
AU - Ueda, Y.
AU - Garrel, C.
AU - Nagao, T.
AU - Paltani, S.
AU - Pierre, M.
AU - Toba, Y.
AU - Vignali, C.
N1 - Funding Information:
The authors are grateful to the anonymous referee for a careful reading and helpful feedback. We acknowledge Lucio Chiappetti for the examination of the manuscript. GM acknowledges support by the Agencia Estatal de Investigación, Unidad de Excelencia María de Maeztu, ref. MDM-2017-0765. IG acknowledges financial support by the European Union’s Horizon 2020 programme “XMM2ATHENA” under grant agreement No 101004168. The research leading to these results has received funding (EP and IG) from the European Union’s Horizon 2020 Programme under the AHEAD2020 project (grant agreement n. 871158). XXL is an international project based around an XMM Very Large Programme surveying two 25 deg extragalactic fields at a depth of ∼6 × 10 erg s cm in the [0.5–2] keV band for point like sources. The XXL website is http://irfu.cea.fr/xxl . Multi-band information and spectroscopic follow-up of the X-ray sources are obtained through a number of survey programmes, summarised at http://xxlmultiwave.pbworks.com/ . This research made use of Astropy, a community-developed core Python package for Astronomy ( http://www.astropy.org , Astropy Collaboration 2018). This publication made use of TOPCAT (Taylor et al. 2005) for table manipulations. The plots in this publication were produced using Matplotlib, a Python library for publication quality graphics (Hunter 2007). Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA member states and NASA. This work is based on data from eROSITA, the soft X-ray instrument aboard SRG, a joint Russian-German science mission supported by the Russian Space Agency (Roskosmos), in the interests of the Russian Academy of Sciences represented by its Space Research Institute (IKI), and the Deutsches Zentrum für Luft- und Raumfahrt (DLR). The SRG spacecraft was built by Lavochkin Association (NPOL) and its subcontractors, and is operated by NPOL with support from the Max Planck Institute for Extraterrestrial Physics (MPE). The development and construction of the eROSITA X-ray instrument was led by MPE, with contributions from the Dr. Karl Remeis Observatory Bamberg & ECAP (FAU Erlangen-Nuernberg), the University of Hamburg Observatory, the Leibniz Institute for Astrophysics Potsdam (AIP), and the Institute for Astronomy and Astrophysics of the University of Tübingen, with the support of DLR and the Max Planck Society. The Argelander Institute for Astronomy of the University of Bonn and the Ludwig Maximilians Universität Munich also participated in the science preparation for eROSITA. This research has made use of data obtained from the Chandra Data Archive and the Chandra Source Catalog, and software provided by the Chandra X-ray Center (CXC) in the application packages CIAO and Sherpa. The Hyper Suprime-Cam (HSC) collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University. The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University. Funding was contributed by the FIRST program from the Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS), Japan Science and Technology Agency (JST), the Toray Science Foundation, NAOJ, Kavli IPMU, KEK, ASIAA, and Princeton University. This paper makes use of software developed for the Large Synoptic Survey Telescope. We thank the LSST Project for making their code available as free software at http://dm.lsst.org . This paper is based [in part] on data collected at the Subaru Telescope and retrieved from the HSC data archive system, which is operated by Subaru Telescope and Astronomy Data Center (ADC) at National Astronomical Observatory of Japan. Data analysis was in part carried out with the cooperation of Center for Computational Astrophysics (CfCA), National Astronomical Observatory of Japan. 2 −15 −1 −2
Publisher Copyright:
©
PY - 2022/11/1
Y1 - 2022/11/1
N2 - In this work, our aim is to investigate the star formation rate (SFR) of the host galaxies of active galactic nuclei (AGNs) in the early Universe. To this end, we constructed a sample of 149 luminous (L2-10keV > 1044 erg-s-1) X-ray AGNs at z¥3.5 selected in three fields with different depths and observed areas from the Chandra COSMOS Legacy survey, XMM-XXL North, and eROSITA Final Equatorial-Depth Survey. We built their spectral energy distributions (SED) using the available multi-wavelength photometry from X-rays up to the far-IR. Then, we estimated the stellar mass, M∗, and the SFR of the AGNs using the X-CIGALE SED fitting algorithm. After applying several quality criteria, we ended up with 89 high-z sources. More than half (55%) of the X-ray sample have spectroscopic redshifts. Based on our analysis, our high-z X-ray AGNs live in galaxies with a median M∗ = 5.6×1010 M· and SFR∗≈240 M·yr-1. The majority of the high-z sources (∼89%) were found inside or above the main sequence (MS) of star-forming galaxies. Estimations of the normalised SFR, SFRNORM, defined as the ratio of the SFR of AGNs, to the SFR of MS galaxies, show that the SFR of AGNs is enhanced by a factor of ∼1.8 compared to non-AGN star-forming systems. Combining our results with previous studies at lower redshifts, we confirmed that SFRNORM does not evolve with redshift. Using the specific black hole accretion rate (i.e. LX divided by M∗), λBHAR, which can be used as a tracer of the Eddington ratio, we found that the majority of AGNs that lie inside or above the MS have higher specific accretion rates compared to sources below the MS. Finally, we found indications that the SFR of the most massive AGN host galaxies (log(M∗/M·) > 1011.5-12) remains roughly constant as a function of M∗, in agreement with the SFR of MS star-forming galaxies.
AB - In this work, our aim is to investigate the star formation rate (SFR) of the host galaxies of active galactic nuclei (AGNs) in the early Universe. To this end, we constructed a sample of 149 luminous (L2-10keV > 1044 erg-s-1) X-ray AGNs at z¥3.5 selected in three fields with different depths and observed areas from the Chandra COSMOS Legacy survey, XMM-XXL North, and eROSITA Final Equatorial-Depth Survey. We built their spectral energy distributions (SED) using the available multi-wavelength photometry from X-rays up to the far-IR. Then, we estimated the stellar mass, M∗, and the SFR of the AGNs using the X-CIGALE SED fitting algorithm. After applying several quality criteria, we ended up with 89 high-z sources. More than half (55%) of the X-ray sample have spectroscopic redshifts. Based on our analysis, our high-z X-ray AGNs live in galaxies with a median M∗ = 5.6×1010 M· and SFR∗≈240 M·yr-1. The majority of the high-z sources (∼89%) were found inside or above the main sequence (MS) of star-forming galaxies. Estimations of the normalised SFR, SFRNORM, defined as the ratio of the SFR of AGNs, to the SFR of MS galaxies, show that the SFR of AGNs is enhanced by a factor of ∼1.8 compared to non-AGN star-forming systems. Combining our results with previous studies at lower redshifts, we confirmed that SFRNORM does not evolve with redshift. Using the specific black hole accretion rate (i.e. LX divided by M∗), λBHAR, which can be used as a tracer of the Eddington ratio, we found that the majority of AGNs that lie inside or above the MS have higher specific accretion rates compared to sources below the MS. Finally, we found indications that the SFR of the most massive AGN host galaxies (log(M∗/M·) > 1011.5-12) remains roughly constant as a function of M∗, in agreement with the SFR of MS star-forming galaxies.
KW - Early Universe
KW - Galaxies: Active
KW - Methods: data analysis
KW - Methods: observational
KW - Methods: statistical
KW - X-rays: galaxies
UR - http://www.scopus.com/inward/record.url?scp=85145223720&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85145223720&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/202243502
DO - 10.1051/0004-6361/202243502
M3 - Article
AN - SCOPUS:85145223720
SN - 0004-6361
VL - 667
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A56
ER -