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Results from the High Elevation Antarctic Terahertz (HEAT) telescope on Ridge A

Results from the High Elevation Antarctic Terahertz (HEAT) telescope on Ridge A Craig Kulesa, on behalf of the HEAT and PLATO-R team. The Life Cycle of matter in the Galaxy remains poorly understood. some UV, X-rays. some UV, X-rays. 21 cm radio. ??. ??. visible light.

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Results from the High Elevation Antarctic Terahertz (HEAT) telescope on Ridge A

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  1. Results from the High Elevation Antarctic Terahertz (HEAT) telescope on Ridge A Craig Kulesa, on behalf of the HEAT and PLATO-R team

  2. The Life Cycle of matter in the Galaxy remains poorly understood. some UV, X-rays some UV, X-rays 21 cm radio ?? ?? visible light infrared and mm waves We need to see how material cycles between gas and stars to understand the origin of stars & planets and the evolution of entire galaxies!

  3. Questions we want to answer • How and where are interstellar clouds made, and how long do they live? • Under what conditions do clouds form stars? • How do stars return enriched material back to the Galaxy? • How do these processes sculpt the evolution of galaxies, near and far? We need a new tool to explore the cosmos – to see the universe in a different (far infrared) light

  4. These questions can be well studied in the far-infrared... 158 um [CII] 205 um [NII] 158 um [CII] 158 um [CII] 370 um [CI] 158 um [CII] 370 um [CI] visible light 370 um [CI] and CO 205 um [NII] Large-scale THz imaging and spectroscopy of carbon, nitrogen & oxygen is needed to observe the full life cycle!

  5. Ridge A Ridge A: a site for SCAR • Submillimeter (< 1 THz) observing conditions all of the time • Super-THz (>1 THz) observing conditions 25% of the time • By far the best THz transmission and stability on Earth • You can (usually) land a Twin Otter aircraft there…

  6. High Elevation Antarctic Terahertz (HEAT) telescope prototype telescope deployed in 2012 to Ridge A with PLATO-R

  7. HEAT is... … a 62 cm off-axis Gregorian telescope … with cryogenic heterodyne receivers in the far-infrared (150–600 um) ...performing a focused spectroscopic survey of the Milky Way in its most important THz lines of carbon and oxygen.

  8. Yes! New atmospheric windows open over Ridge A Ridge A, best 25% Ridge A, median Chajnantor, median Mauna Kea, median

  9. GL 4182 CO J=13-12 1497 GHz T(K) First HEAT Observations at 1.5 THz! GL 4176 CO J=13-12 1497 GHz T(K) 3’

  10. High resolution (heterodyne) spectroscopy turns ordinary 2D maps of the sky into a 3D map of the Galaxy... orbital motion Sun

  11. High resolution (heterodyne) spectroscopy turns ordinary 2D maps of the sky into a 3D map of the Galaxy... G330 in [CI] J=2-1 at 809 GHz from HEAT

  12. High resolution (heterodyne) spectroscopy turns ordinary 2D maps of the sky into a 3D map of the Galaxy... G328 G330 in [CI] J=2-1 at 809 GHz from HEAT

  13. Science Results #1: Atomic carbon is pervasive For 40 years, astronomers have used mm-wave CO emission to determine the properties of star forming clouds. HEAT shows that much of the elemental carbon in dark clouds is actually atomic carbon. Implications: - Clouds are fractal, filamentary, complex in structure, letting UV light permeate and keeping more of the cloud's carbon atomic (but hydrogen molecular). - 30 to 50% of molecular gas is bound up in translucent clouds that have been completely missed in CO surveys. - Atomic and ionized carbon will be even more crucial in metal-poor star forming gas – HEAT, GUSTO, and SOFIA observations of the LMC can be used as a template to explore how the very first stars and galaxies formed.

  14. Science Results #2: A first look at Molecular Cloud Formation We have now identified over 900 clouds in the HEAT survey. Of these, about 20 are candidates for cloud formation, due to the different linewidths of CO and [CI], and [CI] being the main reservoir of carbon. Where do these lie in the Galaxy?

  15. Science Results #2: A first look at Molecular Cloud Formation The bulk of clouds are formed in convergent flows at the leading edge of spiral arms! The 4 inter-arm candidates are associated with two superbubbles, and likely the byproduct of stellar-feedback (a local convergence of gas). This is our first look at the statistics of actual forming clouds!

  16. Later this month, the penultimate data release from the project • All THz site-testing data • Ancillary satellite measurements over the entire high plateau • [CI] J=2-1 at 809 GHz • CO 7-6 at 806 GHz • CO 13-12 at 1497 GHz (1.5 THz) • Pointers to ancillary mm-wave CO and HI data http://soral.as.arizona.edu/heat/

  17. What’s next?

  18. Atacama Large Millimeter Array, Band 11 • New science capabilities, benefiting ALMA & JWST. • The main advantages of Ridge A’s  uniquely stable and transparent THz atmosphere are for wide-field spectroscopic mapping and interferometry.    • Wide field spectroscopic imaging: • Witness the full life cycle of interstellar clouds • Understand the origin of Galactic molecular clouds • Constrain the IMF of stars in relation to their parent clouds • Interferometry for 1 THz and beyond: • Witnessing star formation’s smoking gun:  H2D+ is the best probe of cloud core collapse at the outset of star formation, at 1370 GHz • [CII] line emission at low redshift: connecting the ISM and star formation at high-z from ALMA to z=0 observations with SOFIA. • Formation of the first stars: H2 line cooling gives rise to the first stars. The luminous H2 S(1) line could be directly detected at z>10 in Band 11. • Protoplanetary disks:  Completing models of SEDs via continuum measurements of transition disks at 200 um, resolving gas streams around protoplanets.

  19. Antarctic Atacama Large Millimeter Array, Band 11 • New science capabilities, benefiting ALMA & JWST. • The main advantages of Ridge A’s  uniquely stable and transparent THz atmosphere are for wide-field spectroscopic mapping and interferometry.    • Wide field spectroscopic imaging: • Witness the full life cycle of interstellar clouds • Understand the origin of Galactic molecular clouds • Constrain the IMF of stars in relation to their parent clouds • Interferometry for 1 THz and beyond: • Witnessing star formation’s smoking gun:  H2D+ is the best probe of cloud core collapse at the outset of star formation, at 1370 GHz • [CII] line emission at low redshift: connecting the ISM and star formation at high-z from ALMA to z=0 observations with SOFIA. • Formation of the first stars: H2 line cooling gives rise to the first stars. The luminous H2 S(1) line could be directly detected at z>10 in Band 11. • Protoplanetary disks:  Completing models of SEDs via continuum measurements of transition disks at 200 um, resolving gas streams around protoplanets.

  20. Antarctic Atacama Large Millimeter Array, Band 11 • Enabled by: • 4-8 low-cost telescopes of 1.6m aperture with cooled heterodyne receiver (arrays) from 0.5-1.5 THz • 300 to 800W per module, baselines compact: 50 to 100m • A low-cost hybrid correlator using off-the-shelf components • Continued development of low power cryocoolers, sensitivity and stability of detectors at > 1 THz • More solar power, wind, and a study trade between microturbines and diesel. We want to support multi-year operations between servicing missions. • Come see the poster!

  21. Thank you!

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