LOGIN TO YOUR ACCOUNT

Username
Password
Remember Me
Or use your Academic/Social account:

CREATE AN ACCOUNT

Or use your Academic/Social account:

Congratulations!

You have just completed your registration at OpenAire.

Before you can login to the site, you will need to activate your account. An e-mail will be sent to you with the proper instructions.

Important!

Please note that this site is currently undergoing Beta testing.
Any new content you create is not guaranteed to be present to the final version of the site upon release.

Thank you for your patience,
OpenAire Dev Team.

Close This Message

CREATE AN ACCOUNT

Name:
Username:
Password:
Verify Password:
E-mail:
Verify E-mail:
*All Fields Are Required.
Please Verify You Are Human:
fbtwitterlinkedinvimeoflicker grey 14rssslideshare1
Kargaltsev, O.; Schmitt, B. M.; Pavlov, G. G.; Misanovic, Z. (2011)
Languages: English
Types: Preprint
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Candidate supernova remnants G23.5+0.1 and G25.5+0.0 were observed by XMM-Newton in the course of a snap-shot survey of plerionic and composite SNRs in the Galactic plane. In the field of G23.5+0.1, we detected an extended source, ~3' in diameter, which we tentatively interpret as a pulsar-wind nebula (PWN) of the middle-aged radio pulsar B1830-08. Our analysis suggests an association between PSR B1830-08 and the surrounding diffuse radio emission. If the radio emission is due to the SNR, then the pulsar must be significantly younger than its characteristic age. Alternatively, the radio emission may come from a relic PWN. In the field of G25.5+0.0, which contains the extended TeV source HESS J1837-069, we detected the recently discovered young high-energy pulsar J1838-0655 embedded in a PWN with extent of 1.3'. We also detected another PWN candidate (AX J1837.3-0652) with an extent of 2' and unabsorbed luminosity L_(2-10 keV) ~ 4 x 10^33 erg/s at d=7 kpc. The third X-ray source, located within the extent of the HESS J1837-069, has a peculiar extended radio counterpart, possibly a radio galaxy with a double nucleus or a microquasar. We did not find any evidence of the SNR emission in the G25.5+0.0 field. We provide detailed multiwavelength analysis and identifications of other field sources and discuss robustness of the G25.5+0.0 and G23.5+0.1 classifications as SNRs. (abstract abridged)
  • The results below are discovered through our pilot algorithms. Let us know how we are doing!

    • Abdo, A. A., Ackermann, M., Ajello, M., et al. 2009, ApJS, 183, 46 Abdo, A. A., Ackermann, M., Ajello, M., et al. 2010, ApJS, 188, 405 Aharonian, F., Akhperjanian, A. G., Bazer-Bachi, A. R., et al. 2006, ApJ, 636, 777 Avedisova, V. S. 2002, Astronomy Reports, 46, 193 Bamba, A., Ueno, M., Koyama, K., & Yamauchi, S. 2003, ApJ, 589, 253 Bernardini, F., Israel, G. L., Dall'Osso, S., et al. 2009, A&A, 498, 195 Bird, A. J., Bazzano, A., Bassani, L., et al. 2010, ApJS, 186, 1 Blum, R. D., Conti, P. S., & Damineli, A. 2000, AJ, 119, 1860 Butt, Y. M., Combi, J. A., Drake, J., Finley, J. P., Konopelko, A., Lister, M., Rodriguez, J., & Shepherd, D. 2008, MNRAS, 385, 1764
    • Clifton, T. R., & Lyne, A. G. 1986, Nature, 320, 43 Condon, J. J., Cotton, W. D., Greisen, E. W., Yin, Q. F., Perley, R. A., Taylor, G. B., & Broderick, J. J. 1998, AJ, 115, 1693
    • Ebisawa, K., Tsujimoto, M., Paizis, A., et al. 2005, ApJ, 635, 214 Esposito, P., Israel, G. L., Turolla, R., et al. 2011, MNRAS, 416, 205 Gaensler, B. M., & Johnston, S. 1995, MNRAS, 275, L73 Giveon, U., Becker, R. H., Helfand, D. J., & White, R.L. 2005, AJ, 130, 156 Gogus, E., Cusumano, G., Levan, A. J., et al. 2010, ApJ, 718, 331 Gelbord, J. M., Barthelmy, S. D., Baumgartner, W. H., et al. 2010, GRB Coordinates Network, Circular Service, 10526, 1 (2010), 526, 1
    • Getman, K. V., Broos, P. S., Feigelson, E. D., et al. 2011, ApJS, 194, 3 Gotthelf, E. V., & Halpern, J. P. 2008, ApJ, 681, 515 (GH08) Green, D. A. 2009, Bulletin of the Astronomical Society of India, 37, 45 (available on the World-Wide-Web at "http://www.mrao.cam.ac.uk/surveys/snrs/") Helfand, D. J., Becker, R. H., White, R. L., Fallon, A., & Tuttle, S. 2006, AJ, 131, 2525 Hobbs, G., Lyne, A. G., Kramer, M., Martin, C. E., & Jordan, C. 2004, MNRAS, 353, 1311 Hobbs, G., Lorimer, D. R., Lyne, A. G., & Kramer, M. 2005, MNRAS, 360, 974 Jonker, P. G., Bassa, C. G., Nelemans, G., et al. 2011, ApJS, 194, 18 Kaplan, D. L. 2008, 40 Years of Pulsars: Millisecond Pulsars, Magnetars and More, AIP Conf. Proc., 983, 331
    • Kargaltsev, O., & Pavlov, G. G. 2008, in 40 Years of Pulsars: Millisecond Pulsars, Magnetars, and More, eds. C. Bassa, A. Cumming, V. M. Kaspi, & Z. Wang, AIP Conf. Proc., 983, 171 Kargaltsev, O., & Pavlov, G. 2010, in X-ray Astronomy 2009: Present Status, MultiWavelength Approach And Future Perspectives, eds. A. Comastri, M. Cappi, & L. Angelini, AIP Conf. Proc., 1248, 25
  • No related research data.
  • No similar publications.

Share - Bookmark

Funded by projects

  • NSF | Collaborative Research: Uni...
  • NSF | Collaborative Research: Uni...

Cite this article

Collected from