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UMass Holography Receiver on the LMT, Installation July 2008 Sig. horn Ref. horn
LMT 12GHz holography map (inner 32-m) 0.9 m resolution
Page 1 and 2: The Large Millimeter Telescope Davi
Page 3 and 4: The LMT/GTM project The LMT book El
Page 5 and 6: Cosmology at millimeter-wavelengths
Page 7 and 8: Volcán Sierra La Negra (97 o 18’
Page 9 and 10: LMT site Volcán Sierra Negra (Tlil
Page 11 and 12: Monthy-averaged opacity above LMT s
Page 13 and 14: LMT panel segments
Page 15 and 16: Surface Alignment • Inner 32-m in
Page 17 and 18: Effective area of (5-ring) 50m LMT
Page 19 and 20: March 2006
Page 21 and 22: First-light Instrumentation Overvie
Page 23: Future Instrument Development • C
Page 27 and 28: Taurus Molecular Cloud Survey (FCRA
Page 29 and 30: D.2. “How do galaxies arise and m
Page 31 and 32: • 144-pixel Si-Ni spiderweb bolom
Page 33 and 34: . Arp 220 (z=0.018) L FIR = 2x10 12
Page 35 and 36: Comparison of LMT and other facilit
Page 37 and 38: LMT advantage - sensitivity & resol
Page 39 and 40: Resolving the FIR extragalactic bac
Page 41 and 42: LMT Redshift Search Receiver bandwi
Page 43 and 44: Ultra Wideband Redshift Search Rece
Page 45 and 46: Room temp frontend components mount
Page 47 and 48: Beams separated in azimuth with spa
Page 49 and 50: CO (1-0) Survey of Local ULIRGs T s
Page 51 and 52: LMT High-redshift molecular-line sp
Page 53 and 54: Point-source contamination of the S
Page 55 and 56: 12 mJy pt-source + SZ ~ 3 mJy/beam
Page 57 and 58: Lensing the millimeter galaxy popul
Page 59 and 60: Confusion-limit due to SMG populati
Page 61 and 62: SMGs point-sources SZE with pt-sour
Page 63 and 64: Conclusions • LMT (32-m) is neari
Page 65: Conclusions • Increasing likeliho

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