Remember Me
Or use your Academic/Social account:


Or use your Academic/Social account:


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.


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


Verify Password:
Verify E-mail:
*All Fields Are Required.
Please Verify You Are Human:
fbtwitterlinkedinvimeoflicker grey 14rssslideshare1
Verbeek, Kars; Groot, Paul J.; Scaringi, Simone; Casares, Jorge; Corral-Santana, Jesus M.; Deacon, Niall; Drew, Janet E.; Gänsicke, Boris T.; González-Solares, Eduardo; Greimel, Robert; Heber, Ulrich; Napiwotzki, Ralf; Østensen, Roy H.; Steeghs, Danny; Wright, Nicholas J.; Zijlstra, Albert (2013)
Publisher: Oxford University Press
Languages: English
Types: Article
Subjects: Astrophysics - Solar and Stellar Astrophysics, QB460
We present the result of the cross-matching between ultraviolet (UV)-excess sources selected from the UV-Excess Survey of the Northern Galactic Plane (UVEX) and several infrared (IR) surveys (2MASS, UKIDSS and WISE). From the position in the (J − H) versus (H − K) colour–colour diagram, we select UV-excess candidate white dwarfs with an M-dwarf type companion, candidates that might have a lower mass, brown-dwarf type companion and candidates showing an IR-excess only in the K band, which might be due to a debris disc. Grids of reddened DA+dM and sdO+MS/sdB+MS model spectra are fitted to the U, g, r, i, z, J, H, K photometry in order to determine spectral types and estimate temperatures and reddening. From a sample of 964 hot candidate white dwarfs with (g − r) < 0.2, the spectral energy distribution fitting shows that ∼2–4 per cent of the white dwarfs have an M-dwarf companion, ∼2 per cent have a lower-mass companion, and no clear candidates for having a debris disc are found. Additionally, from WISE six UV-excess sources are selected as candidate quasi-stellar objects (QSOs). Two UV-excess sources have a WISE IR-excess showing up only in the mid-IR W3 band of WISE, making them candidate luminous infrared galaxies (LIRGs) or Sbc starburst galaxies.
  • The results below are discovered through our pilot algorithms. Let us know how we are doing!

    • Adelman-McCarthy, J. K.; et al., 2011, yCat 2306, 0A Aihara H., Allende Prieto C., An D., Anderson S.F. Aubourg E., Balbinot E., Beers T.C., et al., 2011, ApJS 193, 29A
    • Augusteijn T., Greimel R., van den Besselaar E.J.M., Groot P.J., Morales-Rueda L., 2008, A&A 486, 843A Barber S.D., Patterson A.J., Kilic L., Leggett S.K., Dufour P., Bloom J.S., Starr D.L., 2012, ApJ 760, 26 Barentsen G., Vink J.S., Drew J.E., Greimel R. et al., 2011, MNRAS 415, 103B
    • Beuermann K, 2006, A&A 460, 783B Blanton M.R. and Roweis S., 2007, AJ 133, 734B Brinkworth C.S., Ga¨nsicke B.T., Marsh T.R., Hoard D.W., Tappert C., 2009, ApJ 696, 1402B
    • Brinkworth C.S., G¨ansicke B.T., Girven J.M., Hoard D.W., Marsh T.R., Parsons S.G., Koester D., 2012, ApJ 750, 86B Cabrera-Lavers A., Bilir S., Ak S., Yaz E., LopezCorredoira M., 2007, A&A 464, 565C Cardelli J.A., Clayton G.C. & Mathis J.S., 1989, ApJ 345, 245
    • Casali M., Adamson A., Alves de Oliveira C., Almaini O., Burch K., Chuter T., Elliot J. et al., 2007, A&A 467, 777C Corradi R. L. M., Valentini M., Munari U., Drew J. E., et al., 2010, A&A 509, 41
    • Corradi R.L.M., Sabin L., Miszalski B., Rodrguez-Gil P., Santander-Garca M., Jones D., Drew J.E. et al., 2011, MNRAS 410, 1349C
    • Cutri R.M., Skrutskie M.F., van Dyk S. et al., 2003, yCat 2246, 0C
    • Cutri R.M. et al., 2012, yCat 2311, 0C Deacon N.R., Groot P.J., Drew J.E., et al., 2009, MNRAS.397, 1685
    • Debes J.H., Hoard D.W., Wachter S., Leisawitz D.T., Cohen M., 2011, ApJS 197, 38D
    • Debes J.H., Walsh K.J., Stark C., 2012, ApJ 747, 148D Debes J.H., Hoard D.W., Kilic M., Wachter S., Leisawitz D.T., Cohen M., Kirkpatrick J.D., Griffith R.L., 2011, ApJ 729, 4D
    • Debes J.H. & Sigurdsson, S., 2002, ApJ 572, 556D Drew J.E., Greimel R., Irwin M., et al., 2005, MNRAS 362, 753 (D05)
    • Dufour P., Kilic M., Fontaine G., Bergeron P., Melis C., Bochanski J., 2012, ApJ 749, 6D
    • Eisenstein D.J., Weinberg D.H., Agol E., Aihara H., Allende Prieto C., Anderson S.F., Arns J.A., Aubourg, E., et al., 2011, AJ 142, 72E
    • Farihi J., G¨ansicke B.T., Steele P.R., Girven J., Burleigh M.R., Breedt E., Koester D., 2012, MNRAS 421, 1635F Farihi J., Becklin E.E. & Zuckerman B., 2005, ApJS 161, 394F
    • G¨ansicke B.T., Koester D., Marsh T.R., RebassaMansergas A., Southworth J., 2008, MNRAS 391L, 103G G¨ansicke, Boris T., 2011, AIPC 1331, 211G G¨ansicke B.T., Marsh T.R., Southworth J., 2007, MNRAS 380L, 35G
    • G¨ansicke B.T., Koester D., Farihi J., Girven J., Parsons S.G., Breedt E., 2012, MNRAS 424, 333G Girven J., G¨ansicke B.T., Steeghs D. & Koester D., 2011, MNRAS 417, 1210G
    • Gonz´alez-Solares E.A., Walton N.A., Greimel R., Drew, J.E., et al., 2008, MNRAS 388, 89
    • Greiss S., Steeghs D., G¨ansicke B.T., Martn E.L., Groot P.J. et al., 2012 AJ 144, 24G
    • Groot P.J., Verbeek K., Greimel R., et al., 2009, MNRAS 399, 323G
    • Gunn J.E., Siegmund W.A., Mannery E.J., Owen R.E., Hull C.L., Leger R.F, Carey L.N. et al., 2006, AJ 131, 2332G
    • Hales, A.S., Barlow M.J., Drew J.E., Unruh Y.C., Greimel R., Irwin M.J., Gonzlez-Solares E., 2009, ApJ 695, 75H Hambly N.C., Collins R.S., Cross N.J.G., Mann R.G., Read M.A., Sutorius E.T.W., Bond I., Bryant J., et al., 2008, MNRAS 384, 637H
    • Heller R., Homeier D., Dreizler S., Oestensen R., 2009, yCat 34960191H
    • Hewett P.C., Warren S.J., Leggett S.K., Hodgkin S.T., Zabot A., Kanaan A., Cid Fernandes R., 2009, ApJ 704L, 93Z
    • Zuckerman B., & Becklin E E., 1987, Natur 330, 138Z
  • No related research data.
  • Discovered through pilot similarity algorithms. Send us your feedback.

Share - Bookmark

Funded by projects

Cite this article