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|Title:||NGC 2276: a remarkable galaxy with a large number of ultraluminous X-ray sources||Authors:||WOLTER, Anna Luisa Maria
|Issue Date:||2015||Journal:||MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY||Number:||448||Issue:||1||First Page:||781||Abstract:||The starbusting, nearby (D = 32.9 Mpc) spiral (Sc) galaxy NGC 2276 belongs to the sparse group dominated by the elliptical galaxy NGC 2300. NGC 2276 is a remarkable galaxy, as it displays a disturbed morphology at many wavelengths. This is possibly due to gravitational interaction with the central elliptical galaxy of the group. Previous ROSAT and XMM-Newton observations resulted in the detection of extended hot gas emission and of a single very bright (̃10<SUP>41</SUP> erg s<SUP>-1</SUP>) ultraluminous X-ray source (ULX) candidate. Here, we report on a study of the X-ray sources of NGC 2276 based on Chandra data taken in 2004. Chandra was able to resolve 16 sources, 8 of which are ULXs, and to reveal that the previous ULX candidate is actually composed of a few distinct objects. We construct the luminosity function of NGC 2276, which can be interpreted as dominated by high-mass X-ray binaries, and estimate the star formation rate (SFR) to be ̃5-15 M<SUB>☉</SUB> yr<SUP>-1</SUP>, consistent with the values derived from optical and infrared observations. By means of numerical simulations, we show that both ram pressure and viscous transfer effects are necessary to produce the distorted morphology and the high SFR observed in NGC 2276, while tidal interaction have a marginal effect.||Acknowledgments:||We thank Stefano Rota and Mattia Villani for their contribution in an earlier stage of the analysis. We thank Ewan O'Sullivan for precious suggestions. We thank Dong-Woo Kim, Mar Mezcua and the referees for useful inputs that helped improve the paper. We acknowledge partial financial support from INAF through grant PRIN-2011-1 (Challenging Ultraluminous X-ray sources: chasing their black holes and formation pathways). MM and AW acknowledge financial support from the Italian Ministry of Education, University and Research (MIUR) through grant FIRB 2012 RBFR12PM1F. PE acknowledges a Fulbright Research Scholar grant administered by the US–Italy Fulbright Commission and is grateful to the Harvard–Smithsonian Center for Astrophysics for hosting him during his Fulbright exchange. (The Fulbright Scholar Program is sponsored by the US Department of State and administered by CIES, a division of IIE.) This research is based on data obtained from the Chandra Data Archive and has made use of software provided by the Chandra X-ray Center (CXC) in the application package ciao . 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 NASA and of the SIMBAD data base, operated at CDS, Strasbourg, France. The Digitized Sky Surveys were produced at the Space Telescope Science Institute under US Government grant NAG W-2166. The simulations were performed with the Lagrange cluster at the Consorzio Interuniversitario Lombardo per L'Elaborazione Automatica (CILEA).||URI:||http://hdl.handle.net/20.500.12386/24028||URL:||https://academic.oup.com/mnras/article/448/1/781/3852135||ISSN:||0035-8711||DOI:||10.1093/mnras/stv054||Bibcode ADS:||2015MNRAS.448..781W||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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