CMB-HD: An Ultra-Deep, High-Resolution Millimeter-Wave Survey Over Half the Sky. (arXiv:1906.10134v1 [astro-ph.CO])

CMB-HD: An Ultra-Deep, High-Resolution Millimeter-Wave Survey Over Half the Sky. (arXiv:1906.10134v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Sehgal_N/0/1/0/all/0/1">Neelima Sehgal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aiola_S/0/1/0/all/0/1">Simone Aiola</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Basu_K/0/1/0/all/0/1">Kaustuv Basu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bryan_S/0/1/0/all/0/1">Sean Bryan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cyr_Racine_F/0/1/0/all/0/1">Francis-Yan Cyr-Racine</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dicker_S/0/1/0/all/0/1">Simon Dicker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferraro_S/0/1/0/all/0/1">Simone Ferraro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fuller_G/0/1/0/all/0/1">George M. Fuller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Han_D/0/1/0/all/0/1">Dongwon Han</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hasselfield_M/0/1/0/all/0/1">Mathew Hasselfield</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holder_G/0/1/0/all/0/1">Gil Holder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jain_B/0/1/0/all/0/1">Bhuvnesh Jain</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnson_B/0/1/0/all/0/1">Bradley Johnson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnson_M/0/1/0/all/0/1">Matthew Johnson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klaassen_P/0/1/0/all/0/1">Pamela Klaassen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Madhavacheril_M/0/1/0/all/0/1">Mathew Madhavacheril</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mascolo_L/0/1/0/all/0/1">Luca Di Mascolo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mauskopf_P/0/1/0/all/0/1">Philip Mauskopf</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meerburg_D/0/1/0/all/0/1">Daan Meerburg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meyers_J/0/1/0/all/0/1">Joel Meyers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mroczkowski_T/0/1/0/all/0/1">Tony Mroczkowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Munchmeyer_M/0/1/0/all/0/1">Moritz Munchmeyer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Naess_S/0/1/0/all/0/1">Sigurd Naess</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nagai_D/0/1/0/all/0/1">Daisuke Nagai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Newburgh_L/0/1/0/all/0/1">Laura Newburgh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nguyen_H/0/1/0/all/0/1">Ho Nam Nguyen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Niemack_M/0/1/0/all/0/1">Michael Niemack</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oppenheimer_B/0/1/0/all/0/1">Benjamin D. Oppenheimer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pierpaoli_E/0/1/0/all/0/1">Elena Pierpaoli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schaan_E/0/1/0/all/0/1">Emmanuel Schaan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Slosar_A/0/1/0/all/0/1">Anze Slosar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Spergel_D/0/1/0/all/0/1">David Spergel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Switzer_E/0/1/0/all/0/1">Eric Switzer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Engelen_A/0/1/0/all/0/1">Alexander van Engelen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wollack_E/0/1/0/all/0/1">Edward Wollack</a>

A millimeter-wave survey over half the sky, that spans frequencies in the
range of 30 to 350 GHz, and that is both an order of magnitude deeper and of
higher-resolution than currently funded surveys would yield an enormous gain in
understanding of both fundamental physics and astrophysics. By providing such a
deep, high-resolution millimeter-wave survey (about 0.5 uK-arcmin noise and 15
arcsecond resolution at 150 GHz), CMB-HD will enable major advances. It will
allow 1) the use of gravitational lensing of the primordial microwave
background to map the distribution of matter on small scales (k~10/hMpc), which
probes dark matter particle properties. It will also allow 2) measurements of
the thermal and kinetic Sunyaev-Zel’dovich effects on small scales to map the
gas density and gas pressure profiles of halos over a wide field, which probes
galaxy evolution and cluster astrophysics. In addition, CMB-HD would allow us
to cross critical thresholds in fundamental physics: 3) ruling out or detecting
any new, light (< 0.1eV), thermal particles, which could potentially be the dark matter, and 4) testing a wide class of multi-field models that could explain an epoch of inflation in the early Universe. Such a survey would also 5) monitor the transient sky by mapping the full observing region every few days, which opens a new window on gamma-ray bursts, novae, fast radio bursts, and variable active galactic nuclei. Moreover, CMB-HD would 6) provide a census of planets, dwarf planets, and asteroids in the outer Solar System, and 7) enable the detection of exo-Oort clouds around other solar systems, shedding light on planet formation. CMB-HD will deliver this survey in 5 years of observing half the sky, using two new 30-meter-class off-axis cross-Dragone telescopes to be located at Cerro Toco in the Atacama Desert. The telescopes will field about 2.4 million detectors (600,000 pixels) in total.

A millimeter-wave survey over half the sky, that spans frequencies in the
range of 30 to 350 GHz, and that is both an order of magnitude deeper and of
higher-resolution than currently funded surveys would yield an enormous gain in
understanding of both fundamental physics and astrophysics. By providing such a
deep, high-resolution millimeter-wave survey (about 0.5 uK-arcmin noise and 15
arcsecond resolution at 150 GHz), CMB-HD will enable major advances. It will
allow 1) the use of gravitational lensing of the primordial microwave
background to map the distribution of matter on small scales (k~10/hMpc), which
probes dark matter particle properties. It will also allow 2) measurements of
the thermal and kinetic Sunyaev-Zel’dovich effects on small scales to map the
gas density and gas pressure profiles of halos over a wide field, which probes
galaxy evolution and cluster astrophysics. In addition, CMB-HD would allow us
to cross critical thresholds in fundamental physics: 3) ruling out or detecting
any new, light (< 0.1eV), thermal particles, which could potentially be the
dark matter, and 4) testing a wide class of multi-field models that could
explain an epoch of inflation in the early Universe. Such a survey would also
5) monitor the transient sky by mapping the full observing region every few
days, which opens a new window on gamma-ray bursts, novae, fast radio bursts,
and variable active galactic nuclei. Moreover, CMB-HD would 6) provide a census
of planets, dwarf planets, and asteroids in the outer Solar System, and 7)
enable the detection of exo-Oort clouds around other solar systems, shedding
light on planet formation. CMB-HD will deliver this survey in 5 years of
observing half the sky, using two new 30-meter-class off-axis cross-Dragone
telescopes to be located at Cerro Toco in the Atacama Desert. The telescopes
will field about 2.4 million detectors (600,000 pixels) in total.

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