MIRAC3-BLINC Magellan results MIRAC4-BLINC plans Static and Deformable Secondaries

1. MIRAC3-BLINC Magellan resultsMIRAC4-BLINC plansStatic and Deformable Secondaries Phil Hinz and Bill Hoffmann Steward Observatory Giovanni Fazio CfA

2. MIRAC3-BLINC

3. MIRAC-BLINC at the MMT and Magellan Telescopes MIRAC-BLINC has been in routine use for mid-IR observations with the MMT and Magellan since June 2000. from N. Smith et al., 2002

4. mid-IR experience at LCO • We have experienced a broad range of conditions which suggest the site can be reasonable for thermal IR work, but it is not uncommon for good optical conditions which are unusable in the infrared. Observing Run λ Sky (% blackbody) Method Aug. 2001 10.3 3% diff. airmass “ 11.7 0.6% “ 18.0 9% “ April 2002 11.7 3% “ May 2002 unusable? (but clear) Aug. 2002 ? March 2003 10.6 ~8-19% (on-off telescope) 11.7 ~4-15%

5. MIRAC3-BLINC Magellan Science Results • constraints of cold dust in eta Carinae (Smith ApJL 2002, AJ 2003) • measured size of dust disk in Cen A (Korovska et al. ApJL 2003) • observed Galactic center to look for X-ray IR flare correlations (Baganoff et al.) • Constrained the existence of warm dust in young stars in Tucanae-Horologium (Mamajek et al. ApJ 2004) • measured size and found gap in HD 100546 with nulling (Liu et al. ApJL 2002) • Observed sizes of nearby Herbig AE disks to help constrain disk evolution. (Liu et al. in prep)

6. MIR Excess Emission: Probing Remnant Disks 0.3-1 AU over time... Mamajek et al. have observed a sample of young stars of the Tucanae-Horologium moving group looking for photometric evidence of warm debris material.

7. HD 100546: A young Solar System? Constructive Null • Disk approximately 25 AU in diameter. • Inclination and PA are consistent with NIR scattered light images (Augureau et al., Pantin et al.) • Disk similar in size at 11 microns and 24.5 microns. • Consistent with an inner hole? (Bouwman et al.) ε Mus HD 100546 10.3 microns (~silicates) 11.7 microns (~PAH) 12.5 microns (continuum) null position angle

8. Press Release from MIRAC- Magellan data

9. MIRAC4 Specifications • Diffraction limited 8-25 micron imaging using a 256x256 Si:As array • Camera backend for BLINC nuller • Change in magnification of 2x • Grism spectroscopy capability • Mechanical cooling

10. MIRAC4 Optical design

12. MIRAC4 Schedule • We plan to carry out AO imaging and nulling interferometry using MIRAC4-BLINC on the MMT through 2007. • MIRAC4-BLINC will be available for campaign observations on Magellan starting in 2007. • Available for permanent Magellan installation once IRIS is available on the MMT and LBTI is completed (estimated to be mid-2008).

13. MIRAC4 status • Optics have been manufactured and received. • Vacuum case and internal mechanisms are being completed. • Mechanical cooler has been ordered and tested • Electronics are being completed by FORCAST team (Herter) at Cornell.

14. MIRAC4 Status vacuum case and radiation shields detector translation stage Mirror cells, and aperture wheel PT refrigerator housing

15. Where can Magellan make the most impact for IR observations? Challenges for a static system: • Gemini has an IR-optimized system with measured emissivity of 2%. • T-RECS is available on Gemini and has demonstrated 0.1 mJy noise level at N band in an hour. Opportunities for a deformable secondary: • GENIE, the VLT nuller is a technology demonstrator planned for 3-5 micron observations. Thus, no southern searches for zodiacal dust are currently being planned. • The southern hemisphere has several nearby, young moving groups which may turn out to be the ideal objects for more detailed studies of how disks assemble into planets. An IR-optimized AO system could provide the key advantage in IR observations, especially related to planet formation.

16. Mid-Infrared Science at Magellan • Similar science to the MIRAC3 campaigns could continue to be carried out with MIRAC4-BLINC at f/11. • A sensitivity improvement will be achieved with an IR-optimized f/15 secondary • A deformable secondary could enable unique mid-IR science in the hemisphere and position Magellan well for future improvements.

17. 5 micron observations of Vega with the MMTAO system PSF level fake 10 Jupiter mass planet at 20 AU 30 MJ Palomar H band limit (Metchev et al.) 20 MJ 10 MJ 5 MJ Keck K band limit Macintosh et al. ) PSF subtraction and unsharp mask

18. Detection of Warm Debris Disks β Pictoris HR 4796A Vega BLINC MMT Observation • • • ξ Lep • Spitzer is currently allowing us to probe the Kuiper belt equivalents around nearby stars. • The warmer material, if much below ~3000 zodis is undectectable without spatial resolution. • mid-IR AO and a modest baseline could allow the detection of dust down to 10-100 zodis. F0 star Stellar flux dust around an A0 star G0 star K0 star Flux in nulled output of (mJy) M0 star Nulled stellar flux Cloud density (zodis)

19. Backup Slides

20. Cryo-Mechanical Design telescope beam 10 micron detector 2 μm detector imaging “channel” nulling “channel” reimaging ellipsoid beam-splitter

21. HD 100546 Disk Structure Typical Protoplanetary disk model HD 100546 model Protoplanetary disk model has a temperature gradient due to stellar heating and accretion A gap in the disk would cause a lack of emission from hot dust. We expect less 10 m emission due to the gap and a larger size. 10 m emission The size at 20 m is expected to be roughly 4 times as large as at 10 m. The size at 20 m for a disk with an inner gap is similar to that at 10 m . 20 m emission The size of the disk as measured by BLINC at 10 and 20 m is consistent with a ~10 AU gap in the disk caused by a massive protoplanet.