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Probing the Dust Structures in the LMC with Light Echoes Guillermo Damke CTIO PIA Program

Probing the Dust Structures in the LMC with Light Echoes Guillermo Damke CTIO PIA Program Mentor: Armin Rest. Outline. Why do we study Light Echoes (LEs)?. Correlations with HI Data. Correlations with IR Data. Relative distances to Dust Structures. Conclusion.

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Probing the Dust Structures in the LMC with Light Echoes Guillermo Damke CTIO PIA Program

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  1. Probing the Dust Structures in the LMC with Light Echoes Guillermo Damke CTIO PIA Program Mentor: Armin Rest

  2. Outline Why do we study Light Echoes (LEs)?. Correlations with HI Data. Correlations with IR Data. Relative distances to Dust Structures. Conclusion.

  3. Why do we study light echo regions? Light Echoes provide us one of the best ways to know the 3-dimensional dust structure. If we know the time of the SN event we can obtain relative distances from SN to the dust structures. From HI data we can obtain the velocity of a region and correlate it with LE position. From IR data we can identify the structure where we observe LE.

  4. HI Data We have an HI data cube of LMC observed in ATCA (Australia Telescope Compact Array). 5 antennas, 22 m each. Field: 10° x 11.5° (1850x2100 pixels). Center: 5h18m00s -68d45m00s fk5. Pixel Scale= 20''/pix. Beam size= 60''.

  5. Integrated HI image HI Data • The cube has 111 slices. Heliocentric velocity ranges from 196 to 378 km/s. (Increment = 1.6 km/s) • The slices were managed separately with our own Perl program. • Velocities were calibrated by reading the WCS of the header images.

  6. HI-Regions Velocity We can measure the velocity of HI in any pixel. We assume that the structure where the echo is produced has a velocity given by the velocity of the peak of HI.

  7. Velocity Scale km/sec 221.0 237.0 253.0 270.0 286.0 303.0 319.0 LE 1 / ATCA HI-Regions Velocity

  8. HI-Regions Velocity

  9. LMC Region / Spitzer IRAC / R: 8.0 μm, G: 5.8 μm, B: 4.5 μm. IR Data • We downloaded Spitzer images for all the LE regions in the Spitzer Science Archive. • The images were obtained with IRAC in 3.6, 4.5, 5.8, 8.0 μm. • Pixel Scale=1.2''/pix.

  10. Velocity Scale km/sec 221.0 237.0 253.0 270.0 286.0 303.0 319.0 LE 1/ Spitzer IRAC / R: 8.0 μm, G: 5.8 μm, B: 4.5 μm. Spitzer IRAC / 8.0 μm LEs as seen by Spitzer • Light Echo 1. • Age: 610 yr.

  11. LEs as seen by Spitzer • Light Echo 2. • Age: 410 yr. Velocity Scale km/sec 221.0 237.0 253.0 270.0 286.0 Spitzer IRAC / 8.0 μm 303.0 LE 2/ Spitzer IRAC / R: 8.0 μm, G: 5.8 μm, B: 4.5 μm. 319.0

  12. Velocity Scale km/sec 221.0 ATCA 237.0 253.0 270.0 286.0 303.0 319.0 LE 3/ Spitzer IRAC / R: 8.0 μm, G: 5.8 μm, B: 4.5 μm. ATCA – INTEGRATED HI IMAGE LEs as seen by Spitzer • Light Echo 3. • Age: 810 yr. HI

  13. Relative Distances to Dust Structures • If we know the time from the supernova event we can obtain relative distances from the supernova. • We assume the distance to LMC of 51200 pc. • The function which give us the relative distance is: • Where: • z is the distance in front of the supernova (pc). • ρ is the projected distance in the sky (pc). • t is the time from the event (year). • c is the speed of light.

  14. Relative Distances to Dust Structures

  15. Relative Distance and HI Velocity

  16. Next Steps To use NN2 method for LE Regions. To obtain surface brightness of LE and correlate it with Spitzer data. Conclusions • LEs give us a great opportunity to know more about the dust structures. • IR images can help us to identify dust structures.

  17. Agradecimientos! - Acknowledgements! I want to thank: • CTIO, for giving me this great opportunity! • Armin, for giving support, the things I've learned and the SuperMACHO Team! • Stella, the observing run was Incredible! and you know you are the best program director! • REU – PIA Students, you are really nice and I will miss you!

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