We propose to continue the renewed INTEGRAL-multiwavelengh monitoring of GRS 1915+105 with the goal to understand the tight connections that exist between the different emitting media, and placed in a broader context, understand accreting-ejecting sources in general. We will still take advantage of the new facilities we included in the past AOs (the Sardinia radio telescope in the radio domain, and NICER at soft X-rays), and take the opportunity of a collaborative effort with the HMXT team, that should start in April 2018 with simultaneous HMXT observations tentatively schedule during our next INTEGRAL pointings. We will also include infrared/optical (Grantecan and ESO) through dedicated proposals. We require 45 ks pointings taken every second revolution, in order to 1) probe the physics of accretion by studying the 0.5--500 keV emission of the source, 2) study the origin of the high variability of GRS 1915+105, 3) understand the connections between accretion and ejection processes, and 4) constrain physical models of emission processes. Points 1) and 2) can be done by looking into the interplay between the soft and hard X-ray emitters (therefore with JEM-X and IBIS), point 3) and 4) needs contemporaneous broad band coverages and timing studies. Besides these specific points this monitoring will allow us to accumulate more data and thus have a better view of the (rather unknown) behaviour of this source beyond 200 keV. It should be noted that GRS 1915+105 lies in a quite crowded field, with many variable sources such as X-ray binaries of all types, the enigmatic microquasar SS 433, and a couple of highly absorbed IGR sources. This survey will also permit all these sources to be studied in a regular manner. Such a monitoring will greatly participate to the INTEGRAL legacy by bringing new data on a dozen of exciting Galactic sources.
Publications
An infrared study of Galactic OH/IR stars - III. Variability properties of the Arecibo sample - Jimenez-Esteban, F. M., Engels, D.,Aguado, D. S.,Gonzalez, J. B.,Garcia-Lario, P. (2021-08-01) http://ui.adsabs.harvard.edu/#abs/2021MNRAS.505.6051J
Diffuse Galactic emission spectrum between 0.5 and 8.0 MeV - Siegert, Thomas, Berteaud, Joanna,Calore, Francesca,Serpico, Pasquale D.,Weinberger, Christoph (2022-04-01) http://ui.adsabs.harvard.edu/#abs/2022A&A...660A.130S
Magnetars and axion-like particles: probes with the hard X-ray spectrum - Fortin, Jean-Francois, Guo, Huai-Ke,Harris, Steven P.,Sheridan, Elijah,Sinha, Kuver (2021-06-01) http://ui.adsabs.harvard.edu/#abs/2021JCAP...06..036F
Primordial black hole dark matter in the context of extra dimensions - Friedlander, Avi, Mack, Katherine J.,Schon, Sarah,Song, Ningqiang,Vincent, Aaron C. (2022-05-01) http://ui.adsabs.harvard.edu/#abs/2022PhRvD.105j3508F
26Al gamma rays from the Galaxy with INTEGRAL/SPI - Pleintinger, Moritz M. M., Diehl, Roland,Siegert, Thomas,Greiner, Jochen,Krause, Martin G. H. (2023-04-01) http://ui.adsabs.harvard.edu/#abs/2023A&A...672A..53P
The efficiency of nuclear burning during thermonuclear (Type I) bursts as a function of accretion rate - Cavecchi, Y., Galloway, D. K.,Goodwin, A. J.,Johnston, Z.,Heger, A. (2020-12-01) http://ui.adsabs.harvard.edu/#abs/2020MNRAS.499.2148C
Temporal Coverage
2019-04-01T06:06:58Z / 2019-11-13T04:07:58Z
Version
1.0
Mission Description
The INTEGRAL (International Gamma-Ray Astrophysics Laboratory) mission, launched by the European Space Agency (ESA) on October 17, 2002, was designed to study high-energy phenomena in the universe. INTEGRAL was operating until february 2025 and it was equipped with three high-energy instruments: the Imager on Board the INTEGRAL Satellite (IBIS), the Spectrometer on INTEGRAL (SPI), and the JEM-X (Joint European Monitor for X-rays). Its Optical Monitoring Camera (OMC) provided optical V-band magnitude measurements, complementing the high-energy observations.
European Space Agency, Rodriguez, 2025, 'Peering through accretion-ejections mechanisms with an INTEGRAL/multi-wavelength GRS 1915+1015 monitoring program', 1.0, European Space Agency, https://doi.org/10.57780/esa-2usrr2g
