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226 results on '"Haberl, A"'

2. The SRG/eROSITA all-sky survey

Author

Merloni, A., primary, Lamer, G., additional, Liu, T., additional, Ramos-Ceja, M. E., additional, Brunner, H., additional, Bulbul, E., additional, Dennerl, K., additional, Doroshenko, V., additional, Freyberg, M. J., additional, Friedrich, S., additional, Gatuzz, E., additional, Georgakakis, A., additional, Haberl, F., additional, Igo, Z., additional, Kreykenbohm, I., additional, Liu, A., additional, Maitra, C., additional, Malyali, A., additional, Mayer, M. G. F., additional, Nandra, K., additional, Predehl, P., additional, Robrade, J., additional, Salvato, M., additional, Sanders, J. S., additional, Stewart, I., additional, Tubín-Arenas, D., additional, Weber, P., additional, Wilms, J., additional, Arcodia, R., additional, Artis, E., additional, Aschersleben, J., additional, Avakyan, A., additional, Aydar, C., additional, Bahar, Y. E., additional, Balzer, F., additional, Becker, W., additional, Berger, K., additional, Boller, T., additional, Bornemann, W., additional, Brüggen, M., additional, Brusa, M., additional, Buchner, J., additional, Burwitz, V., additional, Camilloni, F., additional, Clerc, N., additional, Comparat, J., additional, Coutinho, D., additional, Czesla, S., additional, Dannhauer, S. M., additional, Dauner, L., additional, Dauser, T., additional, Dietl, J., additional, Dolag, K., additional, Dwelly, T., additional, Egg, K., additional, Ehl, E., additional, Freund, S., additional, Friedrich, P., additional, Gaida, R., additional, Garrel, C., additional, Ghirardini, V., additional, Gokus, A., additional, Grünwald, G., additional, Grandis, S., additional, Grotova, I., additional, Gruen, D., additional, Gueguen, A., additional, Hämmerich, S., additional, Hamaus, N., additional, Hasinger, G., additional, Haubner, K., additional, Homan, D., additional, Ider Chitham, J., additional, Joseph, W. M., additional, Joyce, A., additional, König, O., additional, Kaltenbrunner, D. M., additional, Khokhriakova, A., additional, Kink, W., additional, Kirsch, C., additional, Kluge, M., additional, Knies, J., additional, Krippendorf, S., additional, Krumpe, M., additional, Kurpas, J., additional, Li, P., additional, Liu, Z., additional, Locatelli, N., additional, Lorenz, M., additional, Müller, S., additional, Magaudda, E., additional, Mannes, C., additional, McCall, H., additional, Meidinger, N., additional, Michailidis, M., additional, Migkas, K., additional, Muñoz-Giraldo, D., additional, Musiimenta, B., additional, Nguyen-Dang, N. T., additional, Ni, Q., additional, Olechowska, A., additional, Ota, N., additional, Pacaud, F., additional, Pasini, T., additional, Perinati, E., additional, Pires, A. M., additional, Pommranz, C., additional, Ponti, G., additional, Poppenhaeger, K., additional, Pühlhofer, G., additional, Rau, A., additional, Reh, M., additional, Reiprich, T. H., additional, Roster, W., additional, Saeedi, S., additional, Santangelo, A., additional, Sasaki, M., additional, Schmitt, J., additional, Schneider, P. C., additional, Schrabback, T., additional, Schuster, N., additional, Schwope, A., additional, Seppi, R., additional, Serim, M. M., additional, Shreeram, S., additional, Sokolova-Lapa, E., additional, Starck, H., additional, Stelzer, B., additional, Stierhof, J., additional, Suleimanov, V., additional, Tenzer, C., additional, Traulsen, I., additional, Trümper, J., additional, Tsuge, K., additional, Urrutia, T., additional, Veronica, A., additional, Waddell, S. G. H., additional, Willer, R., additional, Wolf, J., additional, Yeung, M. C. H., additional, Zainab, A., additional, Zangrandi, F., additional, Zhang, X., additional, Zhang, Y., additional, and Zheng, X., additional

Published
2024
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4. O Corona, where art thou? eROSITA's view of UV-optical-IR variability-selected massive black holes in low-mass galaxies

Author

Arcodia, R., primary, Merloni, A., additional, Comparat, J., additional, Dwelly, T., additional, Seppi, R., additional, Zhang, Y., additional, Buchner, J., additional, Georgakakis, A., additional, Haberl, F., additional, Igo, Z., additional, Kyritsis, E., additional, Liu, T., additional, Nandra, K., additional, Ni, Q., additional, Ponti, G., additional, Salvato, M., additional, Ward, C., additional, Wolf, J., additional, and Zezas, A., additional

Published
2023
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5. Abundance and temperature of the outer hot circumgalactic medium

Author

Ponti, G., primary, Zheng, X., additional, Locatelli, N., additional, Bianchi, S., additional, Zhang, Y., additional, Anastasopoulou, K., additional, Comparat, J., additional, Dennerl, K., additional, Freyberg, M., additional, Haberl, F., additional, Merloni, A., additional, Reiprich, T. H., additional, Salvato, M., additional, Sanders, J., additional, Sasaki, M., additional, Strong, A., additional, and Yeung, M. C. H., additional

Published
2023
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7. SRG/eROSITA-triggered XMM-Newton observations of three Be/X-ray binaries in the LMC: Discovery of X-ray pulsations

Author

Haberl, F., primary, Maitra, C., additional, Kaltenbrunner, D., additional, Buckley, D. A. H., additional, Monageng, I. M., additional, Udalski, A., additional, Doroshenko, V., additional, Ducci, L., additional, Kreykenbohm, I., additional, Maggi, P., additional, Rau, A., additional, Vasilopoulos, G., additional, Weber, P., additional, and Wilms, J., additional

Published
2023
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8. Study of the excess Fe XXV line emission in the central degrees of the Galactic centre using XMM-Newton data

Author

Anastasopoulou, K., primary, Ponti, G., additional, Sormani, M. C., additional, Locatelli, N., additional, Haberl, F., additional, Morris, M. R., additional, Churazov, E. M., additional, Schödel, R., additional, Maitra, C., additional, Campana, S., additional, Di Teodoro, E. M., additional, Jin, C., additional, Khabibullin, I., additional, Mondal, S., additional, Sasaki, M., additional, Zhang, Y., additional, and Zheng, X., additional

Published
2023
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10. eRASSt J040515.6 − 745202, an X-ray burster in the Magellanic Bridge

Author

Haberl, F., primary, Vasilopoulos, G., additional, Maitra, C., additional, Valdes, F., additional, Lang, D., additional, Doroshenko, V., additional, Ducci, L., additional, Kreykenbohm, I., additional, Rau, A., additional, Weber, P., additional, Wilms, J., additional, Maggi, P., additional, Bailyn, C. D., additional, Jaisawal, G. K., additional, Ray, P. S., additional, and Treiber, H., additional

Published
2023
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11. Broadband study and the discovery of pulsations from the Be/X-ray binary eRASSU J052914.9−662446 in the Large Magellanic Cloud

Author

Maitra, C., primary, Kaltenbrunner, D., additional, Haberl, F., additional, Buckley, D. A. H., additional, Monageng, I. M., additional, Udalski, A., additional, Carpano, S., additional, Coley, J. B., additional, Doroshenko, V., additional, Ducci, L., additional, Malacaria, C., additional, König, O., additional, Santangelo, A., additional, Vasilopoulos, G., additional, and Wilms, J., additional

Published
2023
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12. Study of the excess Fe XXV line emission in the central degrees of the Galactic centre using XMM-Newton data

Author

K. Anastasopoulou, G. Ponti, M. C. Sormani, N. Locatelli, F. Haberl, M. R. Morris, E. M. Churazov, R. Schödel, C. Maitra, S. Campana, E. M. Di Teodoro, C. Jin, I. Khabibullin, S. Mondal, M. Sasaki, Y. Zhang, X. Zheng, Ministerio de Ciencia e Innovación (España), European Research Council, and European Commission

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Galaxy: center, Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, X-rays: general, Astrophysics - High Energy Astrophysical Phenomena, Galaxy: bulge, X-rays: ISM, Galaxy: disk
Abstract

This is an Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited., The diffuse Fe XXV (6.7 keV) line emission observed in the Galactic ridge is widely accepted to be produced by a superposition of a large number of unresolved X-ray point sources. In the very central degrees of our Galaxy, however, the existence of an extremely hot (~7 keV) diffuse plasma is still under debate. In this work we measure the Fe XXV line emission using all available XMM-Newton observations of the Galactic centre (GC) and inner disc (−10° < ℓ < 10°, −2° < b < 2°). We use recent stellar mass distribution models to estimate the amount of X-ray emission originating from unresolved point sources, and find that within a region of ℓ = ±1° and b = ±0.25° the 6.7keV emission is 1.3–1.5 times in excess of what is expected from unresolved point sources. The excess emission is enhanced towards regions where known supernova remnants are located, suggesting that at least a part of this emission is due to genuine diffuse very hot plasma. If the entire excess is due to very hot plasma, an energy injection rate of at least ~6 × 1040 erg s−1 is required, which cannot be provided by the measured supernova explosion rate or past Sgr A* activity alone. However, we find that almost the entire excess we observe can be explained by assuming GC stellar populations with iron abundances ~1.9 times higher than those in the bar/bulge, a value that can be reproduced by fitting diffuse X-ray spectra from the corresponding regions. Even in this case, a leftover X-ray excess is concentrated within ℓ = ±0.3° and b = ±0.15°, corresponding to a thermal energy of ~2 × 1052 erg, which can be reproduced by the estimated supernova explosion rate in the GC. Finally we discuss a possible connection to the observed GC Fermi-LAT excess. © The Authors 2023., This project acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme Hot Milk (grant agreement No 865637). K.A. thanks Dimitrios L. Anastassopoulos for the helpful discussions. M.M. acknowledges support from NASA under grant GO1-22138X to UCLA. M.C.S. acknowledges support from the Deutsche Forschungsgemeinschaft (DFG) via the Collaborative Research Center (SFB 881, Project-ID 138713538) “The Milky Way System” (sub-projects A1, B1, B2 and B8) and from the European Research Council in the ERC Synergy Grant “ECOGAL - Understanding our Galactic ecosystem: From the disc of the Milky Way to the formation sites of stars and planets” (project ID 855130). M.S. acknowledges support from the Deutsche Forschungsgemeinschaft through the grants SA 2131/13-1, SA 2131/14-1, and SA 2131/15-1. I.K. acknowledges support by the COMPLEX project from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme grant agreement ERC-2019-AdG 882679. E.D.T. acknowledges support by the MW-WINDS project from the European Research Council (ERC) under grant agreement no. 101040751. We also made use of NASA’s Astrophysics Data System Bibliographic Services.

Published
2023
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13. Cyclotron Lines in Highly Magnetized Neutron Stars

Author

Staubert, R, Trümper, J, Kendziorra, E, Klochkov, D, Postnov, K, Kretschmar, P, Pottschmidt, K, Haberl, F, Rothschild, R.E, Santangelo, A, Wilms, J, Kreykenbohm, I, and Fürst, F

Subjects
Astrophysics
Abstract

Cyclotron lines, also called cyclotron resonant scattering features are spectral features, generally appearing in absorption, in the X-ray spectra of objects containing highly magnetized neutron stars, allowing the direct measurement of the magnetic field strength in these objects. Cyclotron features are thought to be due to resonant scattering of photons by electrons in the strong magnetic fields. The main content of this contribution focusses on electron cyclotron lines as found in accreting X-ray binary pulsars (XRBP) with magnetic fields on the order of several 1012 Gauss. Also, possible proton cyclotron lines from single neutron stars with even stronger magnetic fields are briefly discussed. With regard to electron cyclotron lines, we present an updated list of XRBPs that show evidence of such absorption lines. The first such line was discovered in a 1976 balloon observation of the accreting binary pulsar Hercules X-1, it is considered to be the first direct measurement of the magnetic field of a neutron star. As of today (end 2018), we list 35 XRBPs showing evidence of one ore more electron cyclotron absorption line(s). A few have been measured only once and must be confirmed (several more objects are listed as candidates). In addition to the Tables of objects, we summarize the evidence of variability of the cyclotron line as a function of various parameters (especially pulse phase, luminosity and time), and add a discussion of the different observed phenomena and associated attempts of theoretical modeling. We also discuss our understanding of the underlying physics of accretion onto highly magnetized neutron stars. For proton cyclotron lines, we present tables with seven neutron stars and discuss their nature and the physics in these objects.

Published
2019
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15. The eROSITA Final Equatorial Depth Survey (eFEDS)

Author

Comparat, Johan, primary, Truong, Nhut, additional, Merloni, Andrea, additional, Pillepich, Annalisa, additional, Ponti, Gabriele, additional, Driver, Simon, additional, Bellstedt, Sabine, additional, Liske, Joe, additional, Aird, James, additional, Brüggen, Marcus, additional, Bulbul, Esra, additional, Davies, Luke, additional, Villalba, Justo Antonio González, additional, Georgakakis, Antonis, additional, Haberl, Frank, additional, Liu, Teng, additional, Maitra, Chandreyee, additional, Nandra, Kirpal, additional, Popesso, Paola, additional, Predehl, Peter, additional, Robotham, Aaron, additional, Salvato, Mara, additional, Thorne, Jessica E., additional, and Zhang, Yi, additional

Published
2022
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16. XMM-Newton and SRG/eROSITA observations of the isolated neutron star candidate 4XMM J022141.5−735632

Author

Pires, A. M., primary, Motch, C., additional, Kurpas, J., additional, Schwope, A. D., additional, Valdes, F., additional, Haberl, F., additional, Traulsen, I., additional, Tubín, D., additional, Becker, W., additional, Comparat, J., additional, Maitra, C., additional, Meisner, A., additional, Moustakas, J., additional, and Salvato, M., additional

Published
2022
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17. The eROSITA extragalactic CalPV serendipitous catalog

Author

Liu, Teng, primary, Merloni, Andrea, additional, Wolf, Julien, additional, Salvato, Mara, additional, Reiprich, Thomas H., additional, Comparat, Johan, additional, Arcodia, Riccardo, additional, Lamer, Georg, additional, Georgakakis, Antonis, additional, Dwelly, Tom, additional, Sanders, Jeremy, additional, Buchner, Johannes, additional, Haberl, Frank, additional, Ramos-Ceja, Miriam E., additional, Wilms, Jörn, additional, Nandra, Kirpal, additional, Brunner, Hermann, additional, Brusa, Marcella, additional, Schwope, Axel, additional, Robrade, Jan, additional, Freyberg, Michael, additional, Boller, Thomas, additional, Maitra, Chandreyee, additional, Veronica, Angie, additional, and Malyali, Adam, additional

Published
2022
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20. SRG/eROSITA-triggered XMM-Newton observations of three Be/X-ray binaries in the LMC: Discovery of X-ray pulsations

Author

F. Haberl, C. Maitra, D. Kaltenbrunner, D. A. H. Buckley, I. M. Monageng, A. Udalski, V. Doroshenko, L. Ducci, I. Kreykenbohm, P. Maggi, A. Rau, G. Vasilopoulos, P. Weber, and J. Wilms

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

Using data from eROSITA, the soft X-ray instrument aboard Spectrum-Roentgen-Gamma (SRG), we report the discovery of two new hard transients, eRASSU J050810.4-660653 and eRASSt J044811.1-691318, in the Large Magellanic Cloud. We also report the detection of the Be/X-ray binary RX J0501.6-7034 in a bright state. We initiated follow-up observations to investigate the nature of the new transients and to search for X-ray pulsations coming from RX J0501.6-7034. We analysed the X-ray spectra and light curves from our XMM-Newton observations, obtained optical spectra using the South African Large Telescope to look for Balmer emission lines and utilised the archival data from the Optical Gravitational Lensing Experiment (OGLE) for the long-term monitoring of the optical counterparts. We find X-ray pulsations for eRASSU J050810.4-660653, RX J0501.6-7034, and eRASSt J044811.1-691318 of 40.6 s, 17.3 s, and 784 s, respectively. The Halpha emission lines with equivalent widths of -10.4 A (eRASSU J050810.4-660653) and -43.9 A (eRASSt J044811.1-691318) were measured, characteristic for a circumstellar disc around Be stars. The OGLE I- and V-band light curves of all three systems exhibit strong variability. A regular pattern of deep dips in the light curves of RX J0501.6-7034 suggests an orbital period of ~451 days. We identify the two new hard eROSITA transients eRASSU J050810.4-660653 and eRASSt J044811.1-691318 and the known Be/X-ray binary RX J0501.6-7034 as Be/X-ray binary pulsars., Accepted for publication in Astronomy & Astrophysics

Published
2023

23. The eROSITA Final Equatorial-Depth Survey (eFEDS)

Author

Vulic, N., primary, Hornschemeier, A. E., additional, Haberl, F., additional, Basu-Zych, A. R., additional, Kyritsis, E., additional, Zezas, A., additional, Salvato, M., additional, Ptak, A., additional, Bogdan, A., additional, Kovlakas, K., additional, Wilms, J., additional, Sasaki, M., additional, Liu, T., additional, Merloni, A., additional, Dwelly, T., additional, Brunner, H., additional, Lamer, G., additional, Maitra, C., additional, Nandra, K., additional, and Santangelo, A., additional

Published
2022
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24. SRGA J124404.1–632232/SRGU J124403.8–632231: New X-ray pulsar discovered in the all-sky survey by the SRG

Author

Doroshenko, V., primary, Staubert, R., additional, Maitra, C., additional, Rau, A., additional, Haberl, F., additional, Santangelo, A., additional, Schwope, A., additional, Wilms, J., additional, Buckley, D. A. H., additional, Semena, A., additional, Mereminskiy, I., additional, Lutovinov, A., additional, Gromadzki, M., additional, Townsend, L. J., additional, and Monageng, I. M., additional

Published
2022
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25. Phase-resolved X-ray spectroscopy of PSR B0656+14 with SRG/eROSITA andXMM-Newton

Author

Schwope, Axel, primary, Pires, Adriana M., additional, Kurpas, Jan, additional, Doroshenko, Victor, additional, Suleimanov, Valery F., additional, Freyberg, Michael, additional, Becker, Werner, additional, Dennerl, Konrad, additional, Haberl, Frank, additional, Lamer, Georg, additional, Maitra, Chandreyee, additional, Potekhin, Alexander Y., additional, Ramos-Ceja, Miriam E., additional, Santangelo, Andrea, additional, Traulsen, Iris, additional, and Werner, Klaus, additional

Published
2022
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26. eROSITA detection of flares from the Be/X-ray binary A0538-66

Author

Ducci, L., primary, Mereghetti, S., additional, Santangelo, A., additional, Ji, L., additional, Carpano, S., additional, Covino, S., additional, Doroshenko, V., additional, Haberl, F., additional, Maitra, C., additional, Kreykenbohm, I., additional, and Udalski, A., additional

Published
2022
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28. The eROSITA Final Equatorial Depth Survey (eFEDS)

Author

Brunner, H., primary, Liu, T., additional, Lamer, G., additional, Georgakakis, A., additional, Merloni, A., additional, Brusa, M., additional, Bulbul, E., additional, Dennerl, K., additional, Friedrich, S., additional, Liu, A., additional, Maitra, C., additional, Nandra, K., additional, Ramos-Ceja, M. E., additional, Sanders, J. S., additional, Stewart, I. M., additional, Boller, T., additional, Buchner, J., additional, Clerc, N., additional, Comparat, J., additional, Dwelly, T., additional, Eckert, D., additional, Finoguenov, A., additional, Freyberg, M., additional, Ghirardini, V., additional, Gueguen, A., additional, Haberl, F., additional, Kreykenbohm, I., additional, Krumpe, M., additional, Osterhage, S., additional, Pacaud, F., additional, Predehl, P., additional, Reiprich, T. H., additional, Robrade, J., additional, Salvato, M., additional, Santangelo, A., additional, Schrabback, T., additional, Schwope, A., additional, and Wilms, J., additional

Published
2022
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29. First studies of the diffuse X-ray emission in the Large Magellanic Cloud with eROSITA

Author

Sasaki, Manami, primary, Knies, Jonathan, additional, Haberl, Frank, additional, Maitra, Chandreyee, additional, Kerp, Jürgen, additional, Bykov, Andrei M., additional, Dennerl, Konrad, additional, Filipović, Miroslav D., additional, Freyberg, Michael, additional, Koribalski, Bärbel S., additional, Points, Sean, additional, and Staveley-Smith, Lister, additional

Published
2022
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31. Three new high-mass X-ray binaries in the Large Magellanic Cloud

Author

F. Haberl, C. Maitra, G. Vasilopoulos, P. Maggi, A. Udalski, I. M. Monageng, and D. A. H. Buckley

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

The Magellanic Clouds host a large population of high-mass X-ray binary (HMXB) systems, but although the Large Magellanic Cloud (LMC) is an order of magnitude more massive than the Small Magellanic Cloud, significantly fewer HMXBs are known. We conducted a search for new HMXBs in XMM-Newton observations, which we performed to investigate supernova remnant candidates in the supergiant shells LMC5 and LMC7. The three observed fields are located in regions, which were little explored in X-rays before. We analysed the XMM-Newton data to look for sources with hard X-ray spectrum and counterparts with optical colours and brightness typical for HMXBs. We report the discovery of three new Be/X-ray binaries, two of them showing pulsations in their X-ray flux. With a luminosity of 6.5e34 erg/s, XMMU J045315.1-693242 in LMC7 was relatively X-ray faint. The long-term OGLE I-band light curve of the V = 15.5 mag counterpart suggests a 49.6 day or 24.8 day orbital period for the binary system. XMMU J045736.9-692727, also located in LMC7 was brighter with a luminosity of 5.6e35 erg/s and hard spectrum with a power-law photon index of 0.63. The X-ray flux revealed clear pulsations with a period of 317.7 s. We obtained optical high resolution spectra from the V = 14.2 mag counterpart using the SALT-HRS spectrograph. Halpha and Hbeta were observed in emission with complex line profiles and equivalent widths of -8.0 A and -1.3 A, respectively. The I-band light curve obtained from OGLE shows a series of four strong outbursts followed by a sudden drop in brightness by more than 1 mag within 73-165 days and a recovery to the level before the outbursts. RX J0524.2-6620, previously classified as X-ray binary candidate, is located at the eastern part of LMC5. We report the discovery of 360.7 s pulsations. (abridged), Comment: 14 pages, 22 figures, accepted for publication in Astronomy & Astrophysics

Published
2022

32. The EXTraS project: Exploring the X-ray transient and variable sky

Author

De Luca, A., primary, Salvaterra, R., additional, Belfiore, A., additional, Carpano, S., additional, D’Agostino, D., additional, Haberl, F., additional, Israel, G. L., additional, Law-Green, D., additional, Lisini, G., additional, Marelli, M., additional, Novara, G., additional, Read, A. M., additional, Rodriguez-Castillo, G., additional, Rosen, S. R., additional, Salvetti, D., additional, Tiengo, A., additional, Vianello, G., additional, Watson, M. G., additional, Delvaux, C., additional, Dickens, T., additional, Esposito, P., additional, Greiner, J., additional, Hämmerle, H., additional, Kreikenbohm, A., additional, Kreykenbohm, S., additional, Oertel, M., additional, Pizzocaro, D., additional, Pye, J. P., additional, Sandrelli, S., additional, Stelzer, B., additional, Wilms, J., additional, and Zagaria, F., additional

Published
2021
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33. eROSITA calibration and performance verification phase: High-mass X-ray binaries in the Magellanic Clouds

Author

Konrad Dennerl, Konstantin Postnov, Manami Sasaki, Michael Freyberg, Victor Doroshenko, X. Dai, N. I. Shakura, Andrzej Udalski, Stefania Carpano, Frank Haberl, and Chandreyee Maitra

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Accretion (meteorology), Phase (waves), FOS: Physical sciences, Binary number, Astronomy and Astrophysics, Astrophysics, Light curve, Luminosity, Pulsar, Space and Planetary Science, Small Magellanic Cloud, Astrophysics - High Energy Astrophysical Phenomena, Large Magellanic Cloud
Abstract

During its performance verification phase, the soft X-ray instrument eROSITA aboard the Spektrum-Roentgen-Gamma(SRG) spacecraft observed large regions in the Magellanic Clouds, where almost 40 known high-mass X-ray binaries (HMXBs, including candidates) are located. We looked for new HMXBs in the eROSITA data, searched for pulsations in HMXB candidates and investigated the long-term behaviour of the full sample using archival X-ray and optical data. For sources sufficiently bright, a detailed spectral and temporal analysis of their eROSITA data was performed. A source detection analysis of the eROSITA images in different energy bands provided count rates and upper limits for the remaining sources. We report the discovery of a new Be/X-ray binary in the Large Magellanic Cloud. The transient SRGEt J052829.5-690345 was detected with a 0.2-8.0 keV luminosity of ~10^35 erg/s and exhibits a hard X-ray spectrum, typical for this class of HMXBs. The OGLE I-band light curve of the V~15.7 mag counterpart shows large variations by up to 0.75 mag, which occur quasi periodically with ~511 days. The eROSITA observations of the Small Magellanic Cloud covered 16 Be/X-ray binary pulsars, five of them were bright enough to accurately determine their current pulse period. The pulse periods for SXP 726 and SXP 1323 measured from eROSITA data are ~800 s and ~1006 s, respectively, far away from their discovery periods. Including archival XMM-Newton observations we update the spin-period history of the two long-period pulsars which show nearly linear trends in their period evolution since more than 15 years. The corresponding average spin-down rate for SXP 726 is 4.3 s/yr while SXP 1323 shows spin-up with a rate of -23.2 s/yr. We discuss the spin evolution of the two pulsars in the framework of quasi-spherical accretion., 21 pages, 28 figures, accepted for publication in Astronomy & Astrophysics, First science highlights from SRG/eROSITA

Published
2022

35. Discovery of four super-soft X-ray sources in XMM-Newton observations of the Large Magellanic Cloud

Author

Frank Haberl and Chandreyee Maitra

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Cataclysmic variable star, White dwarf, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Planetary nebula, Galaxy, Stars, symbols.namesake, Space and Planetary Science, Eddington luminosity, symbols, Astrophysics::Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, education, Large Magellanic Cloud, Astrophysics::Galaxy Astrophysics
Abstract

Super-soft X-ray sources were established as a heterogeneous class of objects from observations of the Large Magellanic Cloud (LMC). We have searched for new sources of this class in the X-ray images obtained from the XMM-Newton survey of the LMC and additional archival observations. We first selected candidates by visual inspection of the image, and screened out artefacts which can mimic super-soft X-ray sources as well as bright foreground stars which create optical loading on the CCD image. We finally obtained 4 new super-soft X-ray sources for which we performed detailed X-ray timing and spectral analysis and searched for possible optical counterparts to identify their nature. XMMU J050452.0-683909 is identified as the central star of the planetary nebula SMP LMC21 in the LMC. We suggest XMMU J051854.8-695601 and XMMU J050815.1-691832 as new soft intermediate polars from the nature of their X-ray spectrum. Their estimated absorption-corrected luminosities and the blackbody radii indicate that they are located in our Galaxy, rather than the LMC. We discovered coherent pulsations of 497 s from XMMU J044626.6-692011 which indicates a magnetic cataclysmic variable nature of the source. The location of XMMU J044626.6-692011 in the LMC or our Galaxy is less clear. It could either be a white dwarf in the LMC with nuclear burning on its surface near the Eddington limit, or another soft intermediate polar in our Galaxy. The discovery of new super-soft X-ray sources makes a significant contribution to the known population in our own Galaxy. An observed higher density of sources in the direction of the Magellanic Clouds can likely be explained by the relatively low Galactic column density in their direction as well as a large number of existing observations sensitive at low X-ray energies., Comment: 9 pages, 8 figures, 4 tables; accepted for publication in A&A

Published
2021

37. The eROSITA X-ray telescope on SRG

Author

Predehl, P., primary, Andritschke, R., additional, Arefiev, V., additional, Babyshkin, V., additional, Batanov, O., additional, Becker, W., additional, Böhringer, H., additional, Bogomolov, A., additional, Boller, T., additional, Borm, K., additional, Bornemann, W., additional, Bräuninger, H., additional, Brüggen, M., additional, Brunner, H., additional, Brusa, M., additional, Bulbul, E., additional, Buntov, M., additional, Burwitz, V., additional, Burkert, W., additional, Clerc, N., additional, Churazov, E., additional, Coutinho, D., additional, Dauser, T., additional, Dennerl, K., additional, Doroshenko, V., additional, Eder, J., additional, Emberger, V., additional, Eraerds, T., additional, Finoguenov, A., additional, Freyberg, M., additional, Friedrich, P., additional, Friedrich, S., additional, Fürmetz, M., additional, Georgakakis, A., additional, Gilfanov, M., additional, Granato, S., additional, Grossberger, C., additional, Gueguen, A., additional, Gureev, P., additional, Haberl, F., additional, Hälker, O., additional, Hartner, G., additional, Hasinger, G., additional, Huber, H., additional, Ji, L., additional, Kienlin, A. v., additional, Kink, W., additional, Korotkov, F., additional, Kreykenbohm, I., additional, Lamer, G., additional, Lomakin, I., additional, Lapshov, I., additional, Liu, T., additional, Maitra, C., additional, Meidinger, N., additional, Menz, B., additional, Merloni, A., additional, Mernik, T., additional, Mican, B., additional, Mohr, J., additional, Müller, S., additional, Nandra, K., additional, Nazarov, V., additional, Pacaud, F., additional, Pavlinsky, M., additional, Perinati, E., additional, Pfeffermann, E., additional, Pietschner, D., additional, Ramos-Ceja, M. E., additional, Rau, A., additional, Reiffers, J., additional, Reiprich, T. H., additional, Robrade, J., additional, Salvato, M., additional, Sanders, J., additional, Santangelo, A., additional, Sasaki, M., additional, Scheuerle, H., additional, Schmid, C., additional, Schmitt, J., additional, Schwope, A., additional, Shirshakov, A., additional, Steinmetz, M., additional, Stewart, I., additional, Strüder, L., additional, Sunyaev, R., additional, Tenzer, C., additional, Tiedemann, L., additional, Trümper, J., additional, Voron, V., additional, Weber, P., additional, Wilms, J., additional, and Yaroshenko, V., additional

Published
2021
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39. Deep XMM-Newton observations of the northern disc of M31

Author

Kavanagh, Patrick J., primary, Sasaki, Manami, additional, Breitschwerdt, Dieter, additional, de Avillez, Miguel A., additional, Filipović, Miroslav D., additional, Galvin, Timothy, additional, Haberl, Frank, additional, Hatzidimitriou, Despina, additional, Henze, Martin, additional, Plucinsky, Paul P., additional, Saeedi, Sara, additional, Sokolovsky, Kirill V., additional, and Williams, Benjamin F., additional

Published
2020
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40. The XMM-Newton Survey of the Small Magellanic Cloud

Author

Haberl, F, Sturm, R, Ballet, J, Bomans, D. J, Buckley, D. A. H, Coe, M. J, Corbet, R, Ehle, M, Filipovic, M. D, Gilfanov, M, Hatzidimitriou, D, La Palombara, N, Mereghetti, S, Pietsch, W, Snowden, S, and Tiengo, A

Subjects
Astronomy
Abstract

Context. Although numerous archival XMM-Newton observations existed towards the Small Magellanic Cloud (SMC) before 2009, only a fraction of the whole galaxy had been covered. Aims. Between May 2009 and March 2010, we carried out an XMM-Newton survey of the SMC, to ensure a complete coverage of both its bar and wing. Thirty-three observations of 30 different fields with a total exposure of about one Ms filled the previously missing parts. Methods. We systematically processed all available SMC data from the European Photon Imaging Camera. After rejecting observations with very high background, we included 53 archival and the 33 survey observations. We produced images in five different energy bands. We applied astrometric boresight corrections using secure identifications of X-ray sources and combined all the images to produce a mosaic covering the main body of the SMC. Results. We present an overview of the XMM-Newton observations, describe their analysis, and summarize our first results, which will be presented in detail in follow-up papers. Here, we mainly focus on extended X-ray sources, such as supernova remnants (SNRs) and clusters of galaxies, that are seen in our X-ray images. Conclusions. Our XMM-Newton survey represents the deepest complete survey of the SMC in the 0.15−12.0 keV X-ray band. We propose three new SNRs that have low surface brightnesses of a few 10−14 erg cm−2 s−1 arcmin−2 and large extents. In addition, several known remnants appear larger than previously measured at either X-rays or other wavelengths extending the size distribution of SMC SNRs to larger values.

Published
2012
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41. The unusual behavior of the young X-ray pulsar SXP 1062 during the 2019 outburst

Author

Juri Poutanen, Sergey S. Tsygankov, Frank Haberl, Victor Doroshenko, Chandreyee Maitra, Alexander A. Lutovinov, Alexander A. Mushtukov, Georgios Vasilopoulos, and Andrea Santangelo

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Scattering, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Accretion (astrophysics), Pulsar, Accretion disc, Space and Planetary Science, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, X-ray pulsar
Abstract

We present results of the first dedicated observation of the young X-ray pulsar SXP 1062 in the broad X-ray energy band obtained during its 2019 outburst with the NuSTAR and XMM-Newton observatories. The analysis of the pulse-phase averaged and phase-resolved spectra in the energy band from 0.5 to 70 keV did not reveal any evidence for the presence of a cyclotron line. The spin period of the pulsar was found to have decreased to 979.48+/-0.06 s implying a ~10% reduction compared to the last measured period during the monitoring campaign conducted about five years ago, and is puzzling considering that the system apparently did not show major outbursts ever since. The switch of the pulsar to the spin-up regime supports the common assumption that torques acting on the accreting neutron star are nearly balanced and thus SXP 1062 likely also spins with a period close to the equilibrium value for this system. The current monitoring of the source revealed also a sharp drop of its soft X-ray flux right after the outburst, which is in drastic contrast to the behaviour during the previous outburst when the pulsar remained observable for years with only a minor flux decrease after the end of the outburst. This unexpected off state of the source lasted for at most 20 days after which SXP 1062 returned to the level observed during previous campaigns. We discuss this and other findings in context of the modern models of accretion onto strongly magnetized neutron stars., 7 pages, 6 figures; accepted for publication in A&A

Published
2020

43. Murchison Widefield Array and XMM-Newton observations of the Galactic supernova remnant G5.9+3.1

Author

Onić, D., primary, Filipović, M. D., additional, Bojičić, I., additional, Hurley-Walker, N., additional, Arbutina, B., additional, Pannuti, T. G., additional, Maitra, C., additional, Urošević, D., additional, Haberl, F., additional, Maxted, N., additional, Wong, G. F., additional, Rowell, G., additional, Bell, M. E., additional, Callingham, J. R., additional, Dwarakanath, K. S., additional, For, B.-Q., additional, Hancock, P. J., additional, Hindson, L., additional, Johnston-Hollitt, M., additional, Kapińska, A. D., additional, Lenc, E., additional, McKinley, B., additional, Morgan, J., additional, Offringa, A. R., additional, Porter, L. E., additional, Procopio, P., additional, Staveley-Smith, L., additional, Wayth, R. B., additional, Wu, C., additional, and Zheng, Q., additional

Published
2019
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49. EXTraS discovery of two pulsators in the direction of the LMC

Author

C. Delvaux, Daniele D'Agostino, Andrea Tiengo, Andrzej Udalski, G. A. Rodriguez Castillo, Stefania Carpano, Frank Haberl, A. De Luca, G. Novara, G. L. Israel, Paolo Esposito, Ruben Salvaterra, Georgios Vasilopoulos, ITA, DEU, NLD, POL, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Brightness, stars: cataclysmic variables, Astrophysics::High Energy Astrophysical Phenomena, X-ray binary, stars: emission-line, FOS: Physical sciences, Astrophysics, Binaries: close, Galaxies: star clusters: individual: Large Magellanic Cloud, Galaxies: stellar content, Novae cataclysmic variables, Stars: emission-line Be, Stars: neutron, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Binary pulsar, stars: neutron, X-rays: binaries, Pulsar, 0103 physical sciences, Large Magellanic Cloud, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astronomy and Astrophysics, Light curve, Orbital period, Galaxy, galaxies: individual: Large Magellanic Cloud, stars: binaries: close, Space and Planetary Science, galaxies: stellar content, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The EXTraS project to explore the X-ray Transient and variable Sky searches for coherent signals in the X-ray archival data of XMM-Newton. XMM-Newton performed more than 400 pointed observations in the region of the Large Magellanic Cloud (LMC). We inspected the results of the EXTraS period search to systematically look for new X-ray pulsators in our neighbour galaxy. We analysed the XMM-Newton observations of two sources from the 3XMM catalogue which show significant signals for coherent pulsations. 3XMM J051259.8-682640 was detected as source with hard X-ray spectrum in two XMM-Newton observations, revealing a periodic modulation of the X-ray flux with 956~s. As optical counterpart we identify an early-type star with Halpha emission. The OGLE I-band light curve exhibits a regular pattern with three brightness dips which mark a period of ~1350 d. The X-ray spectrum of 3XMM J051034.6-670353 is dominated by a super-soft blackbody-like emission component (kT ~ 70 eV) which is modulated by nearly 100% with a period of ~1418 s. From GROND observations we suggest a star with r' = 20.9 mag as possible counterpart of the X-ray source. 3XMM J051259.8-682640 is confirmed as a new Be/X-ray binary pulsar in the Large Magellanic Cloud. We discuss the long-term optical period as likely orbital period which would be the longest known from a high-mass X-ray binary. The spectral and temporal properties of the super-soft source 3XMM J051034.6-670353 are very similar to those of RX J0806.3+1527 and RX J1914.4+2456 suggesting that it belongs to the class of double-degenerate polars and is located in our Galaxy rather than in the LMC., Comment: 10 pages, 13 figures, accepted for publication in Astronomy & Astrophysics, new version with minor corrections

Published
2017

50. 1RXS J173021.5-055933: a cataclysmic variable with a fast-spinning magnetic white dwarf

Author

D. de Martino, Frank Haberl, Giorgio Matt, S. P. Littlefair, T. R. Marsh, Boris T. Gaensicke, M. Mouchet, Koji Mukai, Jean-Marc Bonnet-Bidaud, M. Falanga, V. S. Dhillon, Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Centre National de la Recherche Scientifique (CNRS), Dipartimento de Fisica Roma Tre (DF-Roma3), Università degli Studi Roma Tre, Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Università degli Studi Roma Tre = Roma Tre University (ROMA TRE), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), de Martino, D, Matt, Giorgio, Mukai, K, Bonnet Bidaud, Jm, Falanga, M, Gansicke, Bt, Haberl, F, Marsh, Tr, Mouchet, M, Littlefair, Sp, and Dhillon, V.

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cataclysmic variable star, Photoionization, Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Photometry (optics), Intermediate polar, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, QB, white dwarfs, Physics, cataclysmic variables, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], stars: individual: 1RXS J173021.5-055933, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 010308 nuclear & particles physics, Astrophysics (astro-ph), stars: novae, White dwarf, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Light curve, Magnetic field, stars: binaries: close, Space and Planetary Science, Magnetic dipole
Abstract

We present the first X-ray observations with the XMM-Newton and INTEGRAL satellites of the recently discovered cataclysmic variable 1RXSJ173021.5-055933, together with simultaneous UV and coordinated optical photometry aiming at characterising its broad-band temporal and spectral properties and classifying this system as a magnetic one. We find that the X-ray light curve is dominated by the 128s spin period of the accreting white dwarf in contrast to the far-UV range, which turns out to be unmodulated at a 3sigma level. Near-UV and optical pulses are instead detected at twice the spin frequency. We identify the contributions from two accreting poles that imply a moderately inclined dipole field allowing, one pole to dominate at energies at least up to 10keV, and a secondary that instead is negligible above 5keV. X-ray spectral analysis reveals the presence of multiple emission components consisting of optically thin plasma with temperatures ranging from 0.17keV to 60keV and a hot blackbody at ~90eV. The spectrum is also strongly affected by peculiar absorption components consisting of two high-density (~3x10^(21)cm^(-2) and ~2x10^(23)cm^(-2)) intervening columns, plus a warm absorber. The last is detected from an OVII absorption edge at 0.74keV, which suggests that photoionization of pre-shock material is also occurring in this system. The observed properties indicate that the accretor in 1RXSJ173021.5-055933 is a white dwarf with a likely weak magnetic field, thus confirming this cataclysmic variable as an intermediate polar (IP) with one of the most extreme spin-to-orbit period ratios. This system also joins the small group of IPs showing a soft X-ray reprocessed component, suggesting that this characteristics is not uncommon in these systems., 11 pages, 7 figures, accepted for publication in A&A

Published
2008

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