Gaia GraL: Gaia DR2 Gravitational Lens Systems. VII. XMM-Newton Observations of Lensed Quasars

Creators: Connor, Thomas; Stern, Daniel; Krone-Martins, Alberto; Djorgovski, S. G.; Graham, Matthew J.; Walton, Dominic J.; Delchambre, Ludovic; Ducourant, Christine; Teixeira, Ramachrisna; Le Campion, Jean-François; den Brok, Jakob Sebastian; Dobie, Dougal; Galluccio, Laurent; Jalan, Priyanka; Klioner, Sergei A.; Klüter, Jonas; Mahabal, Ashish A.; Negi, Vibhore; Nierenberg, Anna; Petit, Quentin; Scarano, Sergio, Jr.; Slezak, Eric; Sluse, Dominique; Spíndola-Duarte, Carolina; Surdej, Jean; Wambsganss, Joachim; Gaia GraL Team

Abstract

We present XMM-Newton X-ray observations of nine confirmed lensed quasars at 1 ≲ z ≲ 3 identified by the Gaia Gravitational Lens program. Eight systems are strongly detected, with 0.3–8.0 keV fluxes F_(0.3−8.0) ≳ 5 ×10⁻¹⁴ erg cm⁻² s⁻¹. Modeling the X-ray spectra with an absorbed power law, we derive power-law photon indices and 2–10 keV luminosities for the eight detected quasars. In addition to presenting sample properties for larger quasar population studies and for use in planning for future caustic-crossing events, we also identify three quasars of interest: a quasar that shows evidence of flux variability from previous ROSAT observations, the most closely separated individual lensed sources resolved by XMM-Newton, and one of the X-ray brightest quasars known at z > 3. These sources represent the tip of the discoveries that will be enabled by SRG/eROSITA.

Additional Information

© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2021 September 28; revised 2021 December 14; accepted 2021 December 15; published 2022 March 3. The work of T.C. and D.S. was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. T.C.'s research was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Universities Space Research Association under contract with NASA. S.G.D. and M.J.G. acknowledge a partial support from the NASA ADAP grant 16-ADAP16-0232, and the NSF grant AST-1815034. D.J.W. acknowledges support from the Science and Technology Facilities Council (STFC) in the form of an Ernest Rutherford Fellowship (grant ST/N004027/1). L.D. acknowledges support from the ESA PRODEX Programme "Gaia-DPAC QSOs" and from the Belgian Federal Science Policy Office. S.A.K. was partially supported by the German Aerospace Agency (grant 50QG1402). D.S. acknowledges support from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No. 787886). Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. Facility: XMM - Newton X-Ray Multimirror Mission satellite. Software: CIAO (Fruscione et al. 2006), PyFITS (Barrett & Bridgman 1999), SAS (Gabriel et al. 2004), XSPEC (Arnaud 1996).

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