Atacama Large Millimeter/submillimeter Array Karl G. Jansky Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array ngVLA: Reconfigurability.

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Presentation transcript:

Atacama Large Millimeter/submillimeter Array Karl G. Jansky Very Large Array Robert C. Byrd Green Bank Telescope Very Long Baseline Array ngVLA: Reconfigurability and Brightness Sensitivity Jim Condon NRAO, Charlottesville

ngVLA configuration(s) treating the ngVLA as: a telescope for the proposed “transformational science” SKA high ALMA low an Observatory, not just a telescope US RMS Science Futures II

The ngVLA and “Transformational Science” US RMS Science Futures II

The ngVLA as an Observatory … not just a Telescope or Mission SKA high? ALMA low? Everything except SKA and ALMA for several decades? Only remaining imaging array at cm wavelengths Only remaining imaging array in the northern hemisphere The ngVLA must outlast any current science case and all current radio telescopes (e.g., GBT), so don’t design anything out (reconfigurability, low frequencies, sensitivity to very extended sources,…) if at all possible. US RMS Science Futures II

ngVLA “A++” & SKA1-mid configurations US RMS Science Futures II NGVLA Memo No. 5 (Carilli et al. 2015)

ngVLA seen from deg declination US RMS Science Futures II

Wrong Hemisphere? Sources US RMS Science Futures II

Wrong Hemisphere? ALMA & SKA US RMS Science Futures II

ngVLA “A” VLA A-array US RMS Science Futures II

ngVLA “C” US RMS Science Futures II

ngVLA “E” US RMS Science Futures II EVLA E “brings the full collecting area of the EVLA to bear on large-scale features which are too faint or too extended to be seen with the existing VLA configurations”.

VLA antenna configurations US RMS Science Futures II B configuration Four configurations scaled by factors of 3.285, each with a scale-free power-law radial distribution r n ~ n for good ”natural” PSFs, matched (u,v) coverage in different bands (e.g., 20 cm, 6 cm, 2 cm).

ngVLA sensitivity versus resolution (ngVLA Memo #5) 300 ✕ 18 m antennas 2 polarizations Briggs weighting R = 0 Tapering for lower resolution US RMS Science Futures II

ngVLA A++ sensitivity versus resolution US RMS Science Futures II

ngVLA A++: Continuum and masers only US RMS Science Futures II

ngVLA A++: Continuum and masers only US RMS Science Futures II

ngVLA C: Tapering to 1” resolution US RMS Science Futures II 57 / 240 = 0.24 so in C the point-source rms noise is 1 / 0.24 ~ 4 x higher than in A++

ngVLA C: ~ JVLA C US RMS Science Futures II

Summary: The fixed ngVLA configuration in ngVLA memo 5 is well matched to the primary science goals (~10 mas continuum imaging of protoplanetary disks and ~1” line imaging of lines in high-redshift galaxies). The ngVLA is ~60 deg north of many Galactic targets and its complementary arrays, ALMA and SKA; this suggests longer north-south baselines and increases Tsys by ~50 K near the 115 GHz CO line. ngVLA image noise increases from ~ 2.2 x natural in the high-resolution A++ configuration to ~ 9 x natural in the C configuration. The ngVLA must outlast any current science case and all existing radio telescopes (e.g., GBT), so try not to design anything out. If at all practical, the ngVLA should have moveable elements within a few km of the center (D & E configurations) to image extended sources with high sensitivity, image sources with constant resolution at different wavelengths, search for pulsars near Sgr A*, provide a phased array element for VLBI,... A small subarray of tiny dishes may be needed to image the largest sources. US RMS Science Futures II

The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. science.nrao.edu

Spacings < 18 m US RMS Science Futures II