1 / 14

Optical Follow-up for IceCube

Optical Follow-up for IceCube. Marek Kowalski Humboldt University Berlin. The IceCube Neutrino Telescope. IceCube Fact Sheet. IceTop. Instrumented Volumen – 1 km 3 Angular resolution < 1.0° Energy threshold – 100 GeV Completion – 2011 50% completion – 2008.

elyse
Download Presentation

Optical Follow-up for IceCube

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Optical Follow-up for IceCube Marek Kowalski Humboldt University Berlin

  2. The IceCube Neutrino Telescope IceCube Fact Sheet IceTop • Instrumented Volumen – 1 km3 • Angular resolution < 1.0° • Energy threshold – 100 GeV • Completion – 2011 • 50% completion – 2008 AMANDA Construction: 1997 - 2000 IceCube Construction: 2005 - 2011

  3. Optical follow-up optical SN/GRB detection day 1-10 day 0 IceCube Neutrino-Trigger Network of optical telescopes IceCube

  4. Science Motivation Search for transient sources: • Supernova (id: rising lightcurve) • Gamma-Ray Burst (id: afterglow) • Gamma-Dark Bursts (id: orphan afterglows) MK, A. Mohr, Astropart (2007)

  5. Example: Supernovae with mildly relativistic jets Motivation: Gamma-Ray Bursts, polarisation measurments Gravitational Collapse of a massive, rotating star (>25 M): Hard to prove, since jets are absorbed. Neutrino-prediction: 30 Neutrino-Events in 10 s in IceCube for a 10 Mpc distant Supernova. Ando & Beacom, PRL (2005); Razzaque, Meszaros & Waxman, PRL (2005). Simulation: MacFadyen (2000)

  6. Detecting Supernovae

  7. Supernova sensitivity Ando & Beacom PRL2005 Sensitivity can be doubled by follow-up! MK, A. Mohr, Astropart. Phys (2007)

  8. Optical follow-up with ROTSE planedfor April/Mai 2008 (=50% IceCube) ROTSE III • 4 Telescope (USA, Turkey, Australia, Nambia) • Diameter 0.45 m • Median response time: 7 s • FoV: 1.85 x 1.85 • Up to 50 IceCube ToO-Trigger/Year

  9. IceCube80% Error Circle Optical follow-up with ROTSE planedfor April/Mai 2008 (=50% IceCube) ROTSE III • 4 Telescope (USA, Turkey, Australia, Nambia) • Diameter 0.45 m • Median response time: 7 s • FoV: 1.85 x 1.85 • Up to 50 IceCube ToO-Trigger/Year M31 1.85o

  10. A network of robotic telescopes • ROTSE III 4 x 0.45 m FoV: 2 x 2 RoboNet Stella Monet PTF

  11. Conclusion • There is an opportunity for robotic telescopes such as STELLA to work with IceCube and other neutrino telescopes (ANTARES, KM3NET). • For each telescope, only a small amount of time needed.

  12. Error circle: ~60% of IC40 ~80% of IC80 1.85o

  13. Analysing a ROTSE image • 5052 objects identified • Compare to USNO2.0 reference star catalog (match to within pixel) • 83 objects not in the catalog • Of the 83 objects none shows variations larger than 1 mag GRB/SN would be identified as variable object on time-scales of minutes to days GRB afterglow, 500 s late

  14. Summary • Monitoring module for short time scale to complement the run wise monitoring. • Doublet trigger schema exists but not yet optimized. • ROTSE is ready to receive IC triggers (<50/yr); the goal is to have the online software ready for IC40.

More Related