Probing spacetime around Sagittarius A* using modeled VLBI closure phases

R. Fraga-Encinas; M. Mościbrodzka; C. Brinkerink; H. Falcke

doi:10.1051/0004-6361/201527599

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Volume 588 (April 2016)

A&A, 588 (2016) A57

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Table 1

Estimated system equivalent flux densities (SEFD) at 1.3 mm.

Facility acronym	Facility name	Antennas	Diameter	SEFD
			(m)	(Jy)

Hawaii	3 facilities are phased: Caltech Submillimeter Observatory (CSO),
	James Clerk Maxwell Telescope (JCMT) and Submillimeter Array (SMA)	8	23	4900
CARMA	Combined Array for Research in Millimeter Wave Astronomy	8	27	6500
SMTO	Arizona Radio Observatory Submillimeter Telescope	1	10	11 900
LMT	Large Millimeter Telescope	1	32	10 000^a
APEX	Atacama Pathfinder Experiment	1	12	6500
ALMA	Atacama Large Millimeter Array (ALMA)	10	38	500
IRAM-PV	30-m Institut de Radioastronomie Millimétrique telescope on Pico Veleta	1	30	2900
IRAM-PdB	Institut de Radioastronomie Millimétrique interferometer on Plateau de Bure	6	15	1600

Notes. The diameter is the effective aperture when the given number of antennas are phased together. The expected SEFD values for observations of Sgr A* include typical weather conditions and opacities.

^(a)

Upgrades to the dish and receiver will lower the SEFD of the LMT by a factor of ~10.

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